Seismic velocities are an important prerequisite for seismic processing as a method for hydrocarbons accumulations detection. Seismic velocities are often displayed for mutual comparing, improvement checking, they are filtrated and recalculated for its different characteristic determination. This work deals with basic seismic propagation laws, the meaning of velocities in different stages of seismic processing and this theoretical background is followed by a proposition of method for calculating and displaying of stack velocities.

Les supernovas de type Ia (SNIa) sont des objets transitoires, observables pour une durée de quelques mois et dont la luminosité à son maximum équivaut à celle d'une galaxie entière. Une fois standardisées (c'est à dire corrigées de leurs principales variabilités), elles représentent, un excellent indicateur de distance et ont permis de mettre en évidence, en 1998, ce que l'on peut représenter comme une accélération de l’expansion de l'Univers. Cette thèse s’intéresse à trois points qui concerne l’étude de la cosmologie par les SNIa :En premier lieu on s'intéresse à la chaîne de production des données et à la qualité des images pour le Large Synoptic Survey Telescope (LSST), qui couvrira un large éventail de domaines scientifique, y compris l'observation des SNIa. Actuellement en préparation pour LSST (dont les observations commenceront en 2020), cette chaîne de production a été testée en effectuant le traitement d’images provenant d’un relevé antérieur (champ profond du CFHT). Les paramètres de qualité astrométriques et photométriques présentent une dispersion légèrement supérieure à celle requise par le cahier de charges du LSST. En ce qui concerne la photométrie, les sources de cette dispersion restent à être comprises. Pour ce qui est de l'astrométrie, la qualité obtenue sera vraisemblablement suffisante lorsque l'ajustement par astrométrie simultanée sera implémenté.Ensuite, on propose une méthode permettant de corriger l'effet induit par les vitesses propres des SNIa se trouvant dans des amas de galaxies. En effet, ces vitesses propres sont particulièrement importantes du fait des interactions gravitationnelles, et perturbent la mesure du décalage spectral cosmologique lié à l'expansion de l'Univers. On a pris en compte un échantillon de 145 SNIa à faible décalage spectral (0,005 < z < 0,123), observées par la collaboration Nearby SuperNova Factory. Parmi ces SNIa, 11 SNIa ont été associées à des amas de galaxies. Ces corrections de vitesses propres ont ainsi permis de diminuer la dispersion sur le diagramme de Hubble de 0,137+/-0,36 mag à 0,130 +/- 0,38 mag, pour les SNIa appartenant à des amas. Bien que le poids de ces corrections soit relativement modeste, on a montré qu'elles sont statistiquement significatives. Ce type de corrections pourraient être prises en considération dans de futures analyses cosmologiques. Enfin on s'intéresse à la question de la détectabilité de possibles anisotropies de l’expansion de l'Univers avec les données de SNIa. Étant donné que la distribution spatiale des données actuelles est connue pour limiter la détection d’une anisotropie dans les distances mesurées des SNIa, on a établi des simulations permettant de déterminer si un effet dipolaire d'amplitude comparable à la borne supérieure des observations actuelles (AD=10-3) pourrait être détecté avec les observations futures du LSST. Plusieurs scénarios ont été considérés, chacun considérant un nombre de SNIa différent. Chacun de ces scénarios est étudié suivant deux variantes correspondant à deux directions, l'une (polaire) pour laquelle la distribution de données de LSST serait la plus symétrique possible, l'autre suivant une direction perpendiculaire à celle-ci (équatoriale). On montre que pour les simulations comportant 5000 SNIa, un dipôle d’amplitude AD=10-3 serait détecté indépendamment de sa direction. On constate que la distance statistique entre les distributions obtenues pour un dipôle simulé et les simulations sans dipôle augmente à mesure que le nombre de SNIa simulées est grand. On constate aussi que cette distance statistique est plus grande pour les dipôles alignés sur la direction équatoriale que pour ceux suivant la direction polaire. (...) / Type Ia supernovae (SNIa) are transient objects, which remains observable in the optical for a period of a few months, and whose luminosity at its maximum is comparable to that of a whole galaxy. They represent, once standardized (i.e. corrected for their main variabilities), an excellent distance indicator and, in 1998, provided the first evidence for the acceleration of the expansion of the Universe. This thesis investigates three points in the cosmological SNIa pipeline:First, we focused on the data processing and the quality of the images for the Large Synoptic Survey Telescope (LSST), that will provide data for a number of cosmological observables, including the observation of SNIa. In preparation for LSST (which will start operations in 2020), we carried out a similar data processing strategy on images from a previous survey (deep field of CFHT) and compared to the required parameters of LSST. A dispersion slightly higher than that required was obtained. For photometry, although this excess is small, the sources of this dispersion remain to be understood. For astrometry, the obtained quality is likely to be sufficient when simultaneous astrometry fitting will be implemented.In a second moment, we propose a method to correct the effect of peculiar velocities of SNIa inside galaxy clusters. Indeed, these velocities ​​are more important in the clusters of galaxies, because of the gravitational interactions, and the measurement of the cosmological redshift related to the expansion of the Universe. These peculiar velocities were corrected using a sample of 145 SNIa with a low spectral shift (0.005<z<0.123), observed by the Nearby SuperNova Factory collaboration. Among these SNIa, 11 SNIa were associated with clusters of galaxies. These corrections made it possible to reduce the dispersion on the Hubble diagram, from 0.137 +/- 0.36 mag (before corrections) to 0.130 +/- 0.38 mag (after corrections), for SNIa belonging to clusters. Although the weight of these corrections is relatively modest, they have been shown to be statistically significant. Such corrections could be taken in account in future cosmological analysis. Finally, we focused on the question of the detectability of potential anisotropies in the expansion of the Universe with SNIa data. Since the spatial distribution of current data is known to limit our capability to detect anisotropies in the SNIa measured distances, simulations were made to determine whether a dipole effect of amplitude comparable to the upper bound of current observations (AD = 10-3) could be detected with future observations of the LSST. Several scenarios were considered, each taking into account a different number of SN. Each of these scenarios is studied according to two variants corresponding to two directions, one (polar) for which the distribution of data of LSST would be as symmetrical as possible, the other in a direction perpendicular to this one (equatorial). It is shown that for simulations with 5000 SNIa, an amplitude dipole AD = 10-3 would be detected independently of its direction. It can be seen that the statistical distance between the distributions obtained for a simulated dipole and the simulations without dipole increases as the number of simulated SNIa is large. We also note that this statistical distance is greater for the scenarios considering the equatorial direction than for the ones following the polar direction.All of the effects mentioned above will have a potential impact future cosmological results. How much these effects will affect our understanding of the complete cosmological model is still an open question, but the results we found in this thesis highlight the importance of further scrutinizing such systematics, whether at the level of the quality of images, systematic environmental effects such as the peculiar velocities ​​of the SNIa or of the cosmology model itself such as for the question of a potentially anisotropic universe.

[pt] Um espectrômetro de massa tipo tempo-de-vôo, montado no Laboratório Nacional de Luz Síncrotron (Campinas - SP), foi utilizado para analisar os íons dessorvidos de uma amostra de amônia condensada (temperaturas de análise: 25 a 150 K) ao ser impactada por fragmentos de fissão do 252Cf. O espectrômetro permite identificar e determinar as abundâncias das espécies iônicas dessorvidas. Quanto à parte teórica, foram feitos cálculos para determinar as estruturas mais estáveis dos agregados de NH3 e para determinar suas dinâmicas de emissão de íons secundários observados na parte experimental. A amônia foi escolhida por sua semelhança com a água, uma molécula muito bem estudada. Outra razão é o atual interesse em determinar a formação de compostos orgânicos nas superfícies de corpos interestelares, uma vez que está comprovada a presença da amônia naquelas superfícies. Nos espectros obtidos observa-se a formação de agregados de amônia que podem ser representados por (NH3)nNHm ± com n = 0-30 e m = 0-5, para íons positivos, e com n = 0- 3 para íons negativos. Uma forma de evidenciar a possibilidade de formação de novos compostos foi realizar experiências com a mistura NH3-CO, com a mesma montagem experimental utilizada para a amônia. Observa-se no espectro obtido (antes da sublimação do CO a 30 K) linhas de massa resultantes de reações primárias que correspondem a íons moleculares híbridos com estrutura CnOmHl+.Os cálculos teóricos referentes às estruturas dos agregados foram realizados través do programa Jaguar 5.5 e Jaguar 6.0. O objetivo é determinar as estruturas mais estáveis dos agregados iônicos da amônia através da teoria DFT (Teoria do Funcional de Densidade) por meio da minimização da energia. Encontrou-se uma relação direta entre as estabilidades determinadas e as abundâncias relativas no espectro de massa. Finalmente foram realizados cálculos com o modelo teórico de dessorção iônica induzida por elétrons. Os resultados de distribuição de velocidades e energias foram comparados com os dados experimentais dos agregados da amônia (n = 0, 4), apresentando uma concordância razoável em valor absoluto, mas moderada em forma. / [en] A time-of-flight mass spectrometer, mounted at the Laboratório National de Luz Síncrotron (Campinas - SP), was used to analyze desorbed ions of a condensed ammonia sample (analyzing temperatures: 25 - 150 K) being impacted by 252Cf fission fragments . The spectrometer allows identifying and determining the relative yields of ionic desorbed species. Besides, it had been made theoretical calculations to determine the most stable cluster structures as well as to determine the emission dynamics of NH3 clusters observed in the experimental part. The ammonia was chosen because of its similarity with the water molecule (very well studied). Another reason is the current interest in determining the organic compounds formation in the interstellar surfaces, now that it is proven the presence of ammonia in those surfaces. The measured spectra show the formation of ammonia clusters that can be represented by (NH3)nNHm ± with n = 0 - 30 and m = 0 - 5 for positive ions, and n = 0 - 3 for negative ones. One way to evidence the formation possibility of new compound is to perform experiments with CO-NH3 mixture samples, using the same experimental set up used for the ammonia. In the spectrum measured before CO sublimation (30 K), mass lines, product of primary reactions, corresponding to hybrid molecular ions having the CnOmHl + structure were observed. Theoretical calculations referring to cluster structures had been carried out using the programs Jaguar 5,5 and Jaguar 6.0. The objective is to determine the most stable structures of the ammonia clusters through the Density Functional Theory (DFT) by means of energy minimizations. A direct relation between the computed stabilities and the relative abundances in the mass spectra was found. Finally calculations with the Secondary Electron Induced Desorption (SEID) model had been carried out. Results of velocity and energy distributions had been compared with the experimental data of ammonia clusters (n = 0, 4), presenting a good agreement in absolute values but moderate agreement in shape.

Esta pesquisa está baseada na execução de duas linhas de refração sísmica profunda de 300 km de extensão (L1-Porangatu e L2-Cavalcante) atravessando de oeste para leste o setor central da Província Tocantins, utilizando em cada linha 120 sismógrafos digitais e explosões com tempo controlado e cargas entre 500 e 1000 kg de explosivos a cada 50 km; foram utilizados receptores GPS para o controle da hora e das coordenadas geográficas dos pontos de registro e de explosões. Esse tipo de experimento, com essas condições é pioneiro no Brasil. Os dados deste experimento, considerados de boa qualidade, permitiram, inicialmente, a elaboração de modelos 1D, para cada tiro, utilizando o programa TTInvers. Estes modelos foram relacionados sucessivamente para representar camadas com características semelhantes em um modelo preliminar para modelagem em 2D, que foi realizada com o programa MacRay. Os modelos 2D obtidos representam o resultado final da distribuição de velocidades sísmicas da crosta sob essas linhas. Estes resultados mostram a crosta sob o setor central da Província Tocantins com espessura variando entre 36 e 43 km, cujos parâmetros estão correlacionados com as principais estruturas geológicas existentes na superfície. Os valores médios de VP e da razão VP/VS na Província Tocantins variam em torno de 6,5 km/s e 1,74, respectivamente, com exceção da faixa de dobras e empurrões cujos valores são 6,3 km/s e 1,73. Sob o Cráton São Francisco esses valores são 6,8 km/s e 1,74. Existem indícios de ter ocorrido uma dupla subducção na Província Tocantins, na porção oriental, com o Cráton São Francisco subduzindo para oeste (em | 760 Ma) e na porção ocidental, com o Cráton Amazônico subduzindo para leste (em | 620 Ma). O modelo gravimétrico, obtido neste trabalho em função do modelo sísmico, se ajusta adequadamente com os dados gravimétricos observados, utilizando densidades teóricas ligeiramente modificadas, dentro dos limites permitidos pela função utilizada para calcular essas densidades com base nos valores de VP deste trabalho. As densidades do manto adotadas para a modelagem levaram em conta as idades Paleoproterozóica, sob o Cráton SãoFrancisco menos denso (3,31 g/cm3) e com maior VP (8,26 km/s), e Neoprotorozóica, sob a Província Tocantins, mais densa (3,34 g/cm3) e com menor VP (8,07 km/s). / This research is based on an execution of two lines of deep seismic refraction of 300 km of extension (L1-Porangatu and L2-Cavalcante), crossing over central sector of Tocantins Province from west to east by using, in each line, 120 digital seismographs and explosions with controlled time and explosive charges between 500 and 1,000 kg in each 50 km; GPS receivers were employed in order to control the time and geographical coordinates from recording and shot points. This kind of experiment under these explained conditions is pioneer in Brazil. Initially experiment data, which have been considered of good quality, allowed the elaboration of 1D models, using TTInvers program. Successive models were related to represent layers with similar characteristics in a preliminary model aiming of modelling in 2D, accomplished with MacRay program. Obtained 2D models represent the final result of seismic velocity distribution from crust beneath L1 and L2 lines. Results show crust under central section of Tocantins Province with thickness varying from 36 to 43 km, and whose parameters are correlated to main geological structures existents in surface. VP as well as VP/VS ratio mean values vary about 6.5 km/s and 1.74, respectively, with the exception of fold-and-thrust belt, whose values are 6.3 km/s and 1.73. Those values reach 6.8 km/s and 1.74 beneath São Francisco craton. There are indicia of double subduction occurred in the eastern portion of Tocantins Province with São Francisco Cráton subducting to west (in | 760 Ma), as well as in the western portion, with Amazon Cráton subducting to east (in | 620 Ma). The gravimetric model, obtained in this work in terms of seismic model, adequately adjusts with observed gravimetric data by using theoretical densities slightly modified, within limits allowed by the function employed to calculating the densities based on VP values achieved from this work. Adopted mantle densities to modelling took in consideration Paleoproterozoic age, beneath São Francisco Cráton, less dense (3.31 g/cm3), and with higher VP (8.26 km/s), as well as Neoproterozoic one, beneath Tocantins Province, denser (3.34 g/cm3), and with lower VP (8.07 km/s).

Processes during the meroplanktonic phase regulate population dynamics for many marine benthic invertebrates. I examined changes in vertical distribution of different meroplanktonic larvae in a coastal embayment during a stable period, at high temporal frequencies and spatial resolutions. Plankton samples were collected at 6 depths (3, 6, 9, 12, 18, 24 m) using a pump, every 2-h over a 36- and a 25-h period, during a spring and neap tide, respectively, concurrently with measures of temperature, salinity, fluorescence and current velocity. For 10 gastropod taxa, larval vertical distribution was mostly related to the thermal structure of the water column. Each of 7 taxonomic groups was found either exclusively near the surface, associated with the fluorescence maximum, or showed diel changes in distribution. These larvae that occupy different depths in the water column exhibit different dispersal potentials. / Biogeographical data contained in this thesis will be submitted to the Oceanographic Biogeographic Information System (OBIS) and may be accessed on-line at http://www.iobis.org

Lors du projet Kerguelen Ocean and Plateau compared Study (KEOPS), la dynamique des particules (vitesses de chute, temps de résidence) et les interactions entre dissous et particules (" boundary scavenging ") ont été étudiées afin de mieux comprendre les mécanismes responsables de la fertilisation naturelle en fer observée sur le plateau des Kerguelen. <br />Notre étude utilise deux radionucléides le 230Th et le 231Pa - tous deux produits de désintégration de l'uranium et très réactifs vis-à-vis des particules - comme traceurs de la dynamique des particules.<br />L'étude des vitesses de chute des particules, estimées à partir des distributions de 230Th a montré que, paradoxalement à son fort export de C, le plateau avait des vitesses de chute des particules plus faibles (S= 500 m.an-1) que les stations du large dans les eaux HNLC (S=800 m.an-1). Ce résultat, assez surprenant, soulève une question quant à la limitation du modèle de scavenging 1D dans le cadre de l'étude de la dynamique des particules des systèmes côte-large et suggère l'utilisation d'un modèle 2D pour reproduire le scavenging de ces régions.<br />Sur le plateau, les fortes concentrations de 231Pa dissous suggèrent que du 231Pa a été relâché lors de la dégradation bactérienne d'agrégats, riches en opale (phase pour laquelle le Pa a une forte affinité).<br />Sur l'escarpement à l'Est du plateau, la diminution des concentrations de 230Th et de 231Pa dissous, concomitante à l'augmentation de leur concentration dans les particules, a montré un intense boundary scavenging le long de la pente du plateau, sous l'effet de couches néphéloïdes ou de re-suspension depuis les sédiments, riches en opale.

Made available in DSpace on 2014-12-17T15:14:57Z (GMT). No. of bitstreams: 1 HidalynTC_TESE.pdf: 3025002 bytes, checksum: 560b594294d11c4905312394b1d53359 (MD5) Previous issue date: 2012-02-16 / Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior / We investigate the cosmology of the vacuum energy decaying into cold dark matter according to thermodynamics description of Alcaniz & Lima. We apply this model to analyze the evolution of primordial density perturbations in the matter that gave rise to the first generation of structures bounded by gravity in the Universe, called Population III Objects. The analysis of the dynamics of those systems will involve the calculation of a differential equation system governing the evolution of perturbations to the case of two coupled fluids (dark matter and baryonic matter), modeled with a Top-Hat profile based in the perturbation of the hydrodynamics equations, an efficient analytical tool to study the properties of dark energy models such as the behavior of the linear growth factor and the linear growth index, physical quantities closely related to the fields of peculiar velocities at any time, for different models of dark energy. The properties and the dynamics of current Universe are analyzed through the exact analytical form of the linear growth factor of density fluctuations, taking into account the influence of several physical cooling mechanisms acting on the density fluctuations of the baryonic component of matter during the evolution of the clouds of matter, studied from the primordial hydrogen recombination. This study is naturally extended to more general models of dark energy with constant equation of state parameter in a flat Universe / Investigamos a cosmologia da energia do v?cuo decaindo em mat?ria escura fria de acordo com a descri??o termodin?mica de Alcaniz & Lima. Aplicamos esse modelo na an?lise da evolu??o de perturba??es de densidade primordiais na mat?ria que deram origem a primeira gera??o de estruturas ligadas pela gravidade no Universo, os chamados Objetos da Popula??o III. A an?lise da din?mica desses sistemas envolver? o c?lculo de um sistema de equa??es diferenciais que governam a evolu??o de perturba??es para o caso de dois fluidos acoplados (mat?ria escura e mat?ria bari?nica), modelados com um perfil Top-Hat baseado na perturba??o das equa??es da hidrodin?mica, uma ferramenta anal?tica eficiente para estudar as propriedades dos modelos de energia escura, como o comportamento do fator de crescimento linear e o ?ndice de crescimento, grandezas f?sicas intimamente relacionadas aos campos de velocidades peculiares em qualquer ?poca, para diferentes modelos de energia escura. As propriedades e a din?mica do Universo atual s?o analisadas atrav?s da forma anal?tica exata do fator de crescimento linear de flutua??es de densidade, levando em considera??o a influ?ncia de v?rios mecanismos f?sicos de esfriamento atuando sobre as flutua??es de densidade da componente bari?nica da mat?ria durante a evolu??o das nuvens de mat?ria, estudadas desde a recombina??o primordial do hidrog?nio. Esse estudo ? naturalmente estendido aos modelos mais gerais de energia escura com o par?metro da equa??o de estado constante em um Universo plano

Esta pesquisa está baseada na execução de duas linhas de refração sísmica profunda de 300 km de extensão (L1-Porangatu e L2-Cavalcante) atravessando de oeste para leste o setor central da Província Tocantins, utilizando em cada linha 120 sismógrafos digitais e explosões com tempo controlado e cargas entre 500 e 1000 kg de explosivos a cada 50 km; foram utilizados receptores GPS para o controle da hora e das coordenadas geográficas dos pontos de registro e de explosões. Esse tipo de experimento, com essas condições é pioneiro no Brasil. Os dados deste experimento, considerados de boa qualidade, permitiram, inicialmente, a elaboração de modelos 1D, para cada tiro, utilizando o programa TTInvers. Estes modelos foram relacionados sucessivamente para representar camadas com características semelhantes em um modelo preliminar para modelagem em 2D, que foi realizada com o programa MacRay. Os modelos 2D obtidos representam o resultado final da distribuição de velocidades sísmicas da crosta sob essas linhas. Estes resultados mostram a crosta sob o setor central da Província Tocantins com espessura variando entre 36 e 43 km, cujos parâmetros estão correlacionados com as principais estruturas geológicas existentes na superfície. Os valores médios de VP e da razão VP/VS na Província Tocantins variam em torno de 6,5 km/s e 1,74, respectivamente, com exceção da faixa de dobras e empurrões cujos valores são 6,3 km/s e 1,73. Sob o Cráton São Francisco esses valores são 6,8 km/s e 1,74. Existem indícios de ter ocorrido uma dupla subducção na Província Tocantins, na porção oriental, com o Cráton São Francisco subduzindo para oeste (em | 760 Ma) e na porção ocidental, com o Cráton Amazônico subduzindo para leste (em | 620 Ma). O modelo gravimétrico, obtido neste trabalho em função do modelo sísmico, se ajusta adequadamente com os dados gravimétricos observados, utilizando densidades teóricas ligeiramente modificadas, dentro dos limites permitidos pela função utilizada para calcular essas densidades com base nos valores de VP deste trabalho. As densidades do manto adotadas para a modelagem levaram em conta as idades Paleoproterozóica, sob o Cráton SãoFrancisco menos denso (3,31 g/cm3) e com maior VP (8,26 km/s), e Neoprotorozóica, sob a Província Tocantins, mais densa (3,34 g/cm3) e com menor VP (8,07 km/s). / This research is based on an execution of two lines of deep seismic refraction of 300 km of extension (L1-Porangatu and L2-Cavalcante), crossing over central sector of Tocantins Province from west to east by using, in each line, 120 digital seismographs and explosions with controlled time and explosive charges between 500 and 1,000 kg in each 50 km; GPS receivers were employed in order to control the time and geographical coordinates from recording and shot points. This kind of experiment under these explained conditions is pioneer in Brazil. Initially experiment data, which have been considered of good quality, allowed the elaboration of 1D models, using TTInvers program. Successive models were related to represent layers with similar characteristics in a preliminary model aiming of modelling in 2D, accomplished with MacRay program. Obtained 2D models represent the final result of seismic velocity distribution from crust beneath L1 and L2 lines. Results show crust under central section of Tocantins Province with thickness varying from 36 to 43 km, and whose parameters are correlated to main geological structures existents in surface. VP as well as VP/VS ratio mean values vary about 6.5 km/s and 1.74, respectively, with the exception of fold-and-thrust belt, whose values are 6.3 km/s and 1.73. Those values reach 6.8 km/s and 1.74 beneath São Francisco craton. There are indicia of double subduction occurred in the eastern portion of Tocantins Province with São Francisco Cráton subducting to west (in | 760 Ma), as well as in the western portion, with Amazon Cráton subducting to east (in | 620 Ma). The gravimetric model, obtained in this work in terms of seismic model, adequately adjusts with observed gravimetric data by using theoretical densities slightly modified, within limits allowed by the function employed to calculating the densities based on VP values achieved from this work. Adopted mantle densities to modelling took in consideration Paleoproterozoic age, beneath São Francisco Cráton, less dense (3.31 g/cm3), and with higher VP (8.26 km/s), as well as Neoproterozoic one, beneath Tocantins Province, denser (3.34 g/cm3), and with lower VP (8.07 km/s).

Un des enjeux de la Directive Cadre sur l'Eau (2000) est de rétablir la migration piscicole aval à travers notamment une baisse de la mortalité des poissons au niveau des turbines des centrales hydroélectriques. Les grilles ichtyocompatibles constituent une des solutions possibles grâce à un arrêt physique des poissons couplé à un guidage vers un exutoire de contournement. Dans ce contexte, nous avons mené une étude expérimentale et numérique afin de caractériser différents types de grilles en termes de pertes de charge et de courantologie. Cela a permis de déterminer d'une part les pertes d'énergie liées à la proximité des barreaux pour diverses configurations et d'autre part les vitesses que les poissons sont susceptibles de rencontrer le long des grilles jusqu'à l'exutoire. Ces deux sujets complémentaires ont été abordés via l'utilisation de deux installations hydrauliques couplées à plusieurs systèmes de mesure adaptés à nos modèles de grille. Des mesures de hauteur d'eau ont permis d'établir des nouvelles lois de pertes de charge tandis que des mesures de vitesse avec des systèmes de vélocimétrie acoustique par effet Doppler (ADV) et de vélocimétrie par images de particules (PIV) ont permis de déterminer les angles pour lesquels les grilles satisfont les critères d'ichtyocompatibilité. Certains points de l'étude, liés à la caractérisation des exutoires notamment, ont été résolus grâce à des simulations numériques avec le logiciel OpenFOAM. L'ensemble des résultats obtenus a permis de dimensionner et de comparer les différentes solutions de grilles dans un cas de prise d'eau réel, soulignant ainsi les avantages et problématiques inhérents à chacune des solutions. / The Water Framework Directive (2000) particularly aimed at restoring the fish downstream migration and at preventing fish from being injured or killed in hydropower plant turbines. Fish-friendly trashracks, which physically stop fish and guide them towards bypasses, are one of the possible solutions.In this context, we have carried out an experimental and numerical study focused on the characterization of head losses and velocity distributions for various kinds of trashrack. This helped to quantify the energy loss due to the narrow bar spacing and to assess the magnitude of velocities that fish may face in different trashrack configurations. Two hydraulic installations coupled with several measurement devices allowed the study of both topics on model trashracks. Water depth measurements resulted in new head loss equations while velocity measurements with acoustic Doppler velocimetry (ADV) and particle image velocimetry (PIV) systems allowed the determination of fish-friendly angles in different trashrack configurations. Some other points of the thesis, concerning for instance bypasses, have been investigated with numerical simulations using OpenFOAM software. All the results allowed the conception and the comparison of various trashrack solutions for a real water intake case, highlighting the advantages and drawbacks relative to each of these solutions.

No description available.