Made available in DSpace on 2014-06-11T19:23:39Z (GMT). No. of bitstreams: 0 Previous issue date: 2007-12-07Bitstream added on 2014-06-13T19:50:38Z : No. of bitstreams: 1 vieira_as_me_ilha.pdf: 1217264 bytes, checksum: cb21063aba699b564242c2fc4b3c3ed4 (MD5) / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / Os escoamentos na superfície livre que se processam sobre forte declividade podem desenvolver instabilidades ao cabo de tempo finito. Tais instabilidades aparecem sob formas de ondas tipo “hydraulic jumps” bem espaçados e são denominadas Roll Waves. Estas ondas, longas e periódicas, podem ser contínuas ou descontínuas; contínuas em problema Shallow Water viscoso e descontínuas para o caso não viscoso. Tal fenômeno pode ser observado tanto em escoamentos naturais como em canais artificiais e vertedouros de barragens. Tratando-se de escoamento de Fluidos não newtonianos, tal fenômeno pode ser visto facilmente em lavas torrenciais, avalanchas ou “debris flows”. Nesta dissertação foram analisados matematicamente e numericamente o comportamento e as condições de existência para a formação de Roll Waves em escoamentos laminares e turbulentos. Em escoamentos turbulentos toma-se como referência os trabalhos realizados por Maciel (2001) numa reologia Binghamiana. Para escoamentos laminares, cita-se o trabalho de Mei (1994) em uma reologia tipo Power Law. No plano numérico, para escoamentos turbulentos, foram utilizadas rotinas do MATLAB® versão 6.5 e, para escoamentos laminares, rotinas em FORTRAN 90; onde pôde-se analisar e comparar resultados para diversas reologias. O foco desta dissertação foi tratar o problema Roll Waves como uma instabilidade na vizinhança do regime uniforme para Fluidos não newtonianos, em regimes turbulentos e laminares. A reologia tratada e representativa de diversos escoamentos na natureza foi a de Herschel Bulkley. A partir desta dissertação deixa-se, como perspectiva futura, um estudo mais aprofundado sob formação de ondas em fluidos hiperconcentrados tipo Herschel Bulkley com abordagem experimental a fim de validar resultados apontados nesta pesquisa. / Flows that happen over strong slope with free surface can develop instabilities after some finite time. Such wave shaped instabilities appear in the flow and are of the type “hydraulic jumps” well spaced and they are called Roll Waves. Those waves are long and periodic, continuous or discontinuous, continuous in viscous Shallow Water problems, and discontinuous for the inviscid case. Roll Waves are uncommon in natural flows, but they are common in man made channels and dams spillway. For flows of non Newtonian fluids such phenomenon can be seen easily in lava torrent, avalanche and debris flow. In this work it were mathematically and numerically analyzed the behavior and the existence conditions for the generation of Roll Waves within laminar and turbulent flows. For turbulent flows it is taken as reference the works done by Maciel (2001) dealing with a Bingham rheology. For laminar flows the reference is the work done by Mei (1994) using a Power Law rheology. Numerically, for turbulent flows it were used MATLAB® 6.5 procedures and for laminar flows FORTRAN 90 procedures were developed. Using these reference procedures it was obtained compared and analyzed results for several rheologies. This work left as future perspective a deeper study about the generation of waves in hipper concentrated fluids such as Herschel Bulkley fluid, with an experimental approach aiming to validate results produced. The focus of this work was to treat the so called Roll Waves problem as an instability in the vicinity of the uniform flow regime for non Newtonian fluids under laminar and turbulent flow regimes. The Herschel Bulkley rheology that was treated in this work is representative of several flows that happen in nature.

A historical review of land tenure systems implemented in the Herschel district, Eastern Cape, South Africa and an analysis of the strengths and weaknesses of each system in conjunction with international experience of land tenure provide guidelines as to what elements could be incorporated in the formulation of a new integrated land tenure system. These guidelines together with the information obtained from a questionnaire survey amongst the Herschel population provide the government of South Africa with a broad outline of an integrated land tenure system that could serve to link the former homelands to the land tenure system that currently operates in the rest of the country thereby removing one of the obstacles to rural development and land redistribution.

É notório que a degradação ambiental vem ao longo do tempo posicionando-se como um dos principais problemas do mundo moderno. Dentre as várias questões do interesse ambiental podemos destacar a ascensão da bolha de metano, em reservatórios hidrelétricos, desde o sedimento anóxico no fundo do reservatório até a interface água atmosfera. Neste contexto, a presente tese vêm propor uma nova modelagem matemática para a ascensão da bolha axissimétrica em fluidos newtonianos/nãonewtonianos e mostrar resultados numéricos simulados. Desta forma, o estado da arte estaria elevado a posição de permitir, via Matemática e Simulação Numérica-Computacional, a análise do transporte de metano em reservatórios de hidrelétricas através da bolha / It is well-known that environmental degradation has come along the time positioning as one of the main problems from modern world. Among several questions of the environmental interest may emphasize the methane bubble rise in hydroelectric reservoirs from the anoxic sediment in the bottom of reservoir until water interface atmosphere. In this context, the current thesis has come to propose a new mathematic modeling to the rise of the axisymmetric bubble in the newtonian/non-newtonian fluids and display numerical results simulated. Therefore, the state of art would be ascended to a position to permit, via Mathematics and Computing-Numeric Simulation, the analysis of transport of methane in hydroelectric reservoirs through of bubble

Des panaches sont connus pour migrer à travers le manteau ductile et quasi-Newtonien ; alors que les dikes se fracturent et se propagent dans la lithosphère solide. Cependant, la lithosphère est en fait visco-élastique. Afin de déterminer ce qui se passe dans ce cas complexe, nous avons réalisé une étude expérimentale et numérique sur le développement de panaches thermiques dans des solutions aqueuses de Carbopol, un gel de polymères formant un réseau continu d'éponges microscopiques. Ce fluide est rhéofluidifiant et présente un seuil de contrainte σ₀, de sorte que l'écoulement ne se produit que si la contrainte locale dépasse cette valeur critique σ₀. En dessous de cette valeur, le fluide agit comme un solide élastique. Les propriétés rhéologiques des solutions peuvent être systématiquement ajustées en variant la concentration de Carbopol. Le dispositif consiste en une source locale de chaleur de puissance constante placée au centre d'une cuve cubique. Selon la valeur du rapport entre la contrainte d'origine thermique et la contrainte seuil, Y₀, on peut observer trois régimes différents. A faible Y₀<Yc₁, aucun mouvement n'est détecté ; tandis que pour Yc₁<Y₀<Yc₂ une cellule se développe, puis évolue vers un panache pour Y₀>Yc₂. Nous montrons que les paramètres critiques (Yc₁,Yc₂) dépendent fortement de la géométrie du chauffage. Des mesures simultanées de température et de champs de vitesse montrent que la morphologie du panache ressemble à un doigt, contrairement à la forme de champignon rencontrée dans les fluides newtoniens. Utilisant des simulations numériques avec une description purement visqueuse, où la rhéologie du fluide est décrite par un modèle de Herschel-Bulkley régularisé, sont suffisantes pour rendre compte de la dynamique du panache. Une étude détaillée des paramètres indiquent que la dynamique du panache est gouvernée par la compétition entre la contrainte seuil, la contrainte induite par la flottabilité et les contraintes visqueuses. Nous avons identifié deux paramètres adimensionnés : le paramètre seuil Ψ comparant la contrainte induite par la flottabilité et la contrainte seuil, et le nombre de Bingham Bi comparant la contrainte seuil et les contraintes visqueuses. Un panache ne peut s'élever que si les deux paramètres sont supercritiques, i.e. la contrainte induite par la flottabilité et les contraintes visqueuses sont plus importantes que la contrainte seuil. Par conséquent, le panache peut s'arrêter avant d'atteindre la surface. Des lois d'échelles dans le conduit du panache ont été déterminées pour la vitesse, la température et la taille de la région cisaillée en régime permanent. Elles décrivent raisonnablement le comportement du conduit bien que seul l'effet rhéofluidifiant soit pris en compte. L'application de ces paramètres adimensionnés à la Terre contraignent significativement la limite de plasticité du manteau et de la lithosphère. La contrainte seuil maximale qui permet à une instabilité thermique de pénétrer dans la lithosphère ou le manteau supérieur est entre 100 kPa et 100 MPa, et elle dépend fortement de la taille et de l'anomalie de densité de l'intrusion. / Plumes are known to migrate through the ductile quasi-Newtonian mantle, while dikes fracture and propagate through the solid lithosphere. However, depending on the timescale, the lithosphere presents solid as well as viscous properties. To determine what happens in the complex case, where instabilities propagate through a visco-elastic matrix, we performed a combined study of laboratory experiments and numerical simulations. Here we investigate the development of thermal plumes in aqueous solutions of Carbopol, a polymer gel, forming a continuous network of micrometric sponges. This fluid is shear thinning and has a yield-stress σ₀, whereby flow occurs only if the local stress exceeds this critical value σ₀. Below this value, the fluid acts as an elastic solid. The rheological properties of the solutions can be systematically varied by varying the Carbopol concentration. The setup consists of a localized heat-source operated at constant power, placed at the centre of a square tank. Depending on the ratio of the thermally induced stresses and the yield stress, Y₀, three different regimes may be obtained. For low Y₀<Yc₁ no motion occurs, whereas for Yc₁<Y₀<Yc₂ a cell develops, that evolves into a plume for Y₀>Yc₂. We show that the critical parameters (Yc₁,Yc₂) strongly depend on the geometry of the heating. Combined temperature and velocity field measurements show that the morphology of the plume resembles a finger, contrary to the mushroom-like shape encountered in Newtonian fluids. Numerical simulations using a purely viscous description, where the rheology of the fluid is described by a regularized Herschel-Bulkley model, are sufficient to capture the plume dynamics. A detailed parametric study shows that the plume dynamics are governed by the interplay between yield stress, buoyancy induced stress and viscous stresses. We identify two non-dimensional parameters: the yield parameter Ψ comparing the buoyancy induced stress to the yield stress, and the Bingham number Bi comparing the yield stress to the viscous stresses. We show that a plume can rise only if both parameters are supercritical, i.e. if buoyancy induced stress and viscous stresses each overcome the yield stress. Therefore the plume may come to a halt before it reaches the surface. We propose scaling laws for the plume stem velocity, temperature and the size of the shear zone in the steady state. We show that the scaling laws describe the behaviour in the plume stem reasonably well, if the yield stress is neglected and only the shear thinning behaviour is taken into account. Applying the non-dimensional parameters to Earth places severe constraints on the strength of mantle and lithosphere. The maximum strength that allows for thermal instabilities to penetrate the lithosphere or upper mantle is in between 100 kPa and 100 MPa, and strongly depends on the size and buoyancy of the anomaly.

Les disques protoplanétaires entourant les jeunes étoiles sont les embryons des systèmes planétaires. A différentes phases de leur évolution, ils peuvent subir d'importantes pertes de masse par photoévaporation : des photons énergétiques, issus de l'étoile centrale ou d'une étoile voisine, chauffe le disque qui perd en masse sous l'échappement des particules. Cependant, ce mécanisme et la physique sous-jacente n'ont que peu été contraints par les observations. Les objectifs de cette thèse sont d'étudier la photoévaporation dans le cas particulier où elle est due à des photons FUV, d'identifier les principaux paramètres physiques (densité, température) et processus (chauffage et refroidissement) impliqués, et d'estimer son impact sur l'évolution dynamique des disques. L'étude repose sur le couplage observations - modélisations des disques photoévaporés par les photons UV en provenance d'étoiles massives proches. Ces objets, appelés "proplyds", ont leur disque entouré d'une large enveloppe nourrie des flots de photoévaporation. A l'aide d'un modèle 1D d'une région de photodissociation, j'ai développé un modèle pour l'émission dans l'infrarouge lointain des proplyds. Ce modèle a été utilisé pour interpréter les observations, issues principalement de Herschel, pour quatre proplyds. Il apparait que les conditions physiques en surface de leur disque sont similaires: une densité de l'ordre de 10 6 par cm cube et une température d'environ 1000 K. Cette température est maintenue par un équilibre dynamique : si la surface se refroidit, la perte de masse diminue et l'enveloppe se réduit. L'atténuation UV produite par l'enveloppe diminue alors et le disque, recevant plus de photons UV, chauffe. La majorité du disque peut s'échapper sous forme de flots de photoévaporation avec des taux de perte de masse de quelques 10 -7 masse solaire par an ou plus, en accord avec les observations précédentes des traceurs du gaz ionisé. A la suite de ce travail, j'ai développé un modèle hydrodynamique 1D pour étudier l'évolution dynamique d'un disque en photoévaporation par un champ de rayonnement externe. [...] / Protoplanetary disks are found around young stars, and represent the embryonic stage of planetary systems. At different phases of their evolution, disks may undergo substantial mass-loss by photoevaporation: energetic photons from the central or a nearby star heat the disk, hence particles can escape the gravitational potential and the disk loses mass. However, this mechanism, and the underlying physics regulating photoevaporation, have not been well constrained by observations so far. The aims of this thesis are to study photoevaporation, in the specific case when it is driven by far-UV photons, to identify the main physical parameters (density, temperature) and processes (gas heating and cooling mechanisms) that are involved, and to estimate its impact on the disk dynamical evolution. The study relies on coupling observations and models of disks being photoevaporated by UV photons coming from neighbouring massive star(s). Those objects, also known as "proplyds", appear as disks surrounded by a large cometary shaped envelope fed by the photoevaporation flows. Using a 1D code of the photodissociation region, I developed a model for the far-IR emission of proplyds. This model was used to interpret observations, mainly obtained with the Herschel Space Observatory, of four proplyds. We found similar physical conditions at their disk surface: a density of the order of 10 6 cm and a temperature about 1000 K. We found that this temperature is maintained by a dynamical equilibrium: if the disk surface cools, its mass-loss rate declines and the surrounding envelope is reduced. Consequently, the attenuation of the UV radiation field by the envelope decreases and the disk surface, receiving more UV photons, heats up. Most of the disk is thus able to escape through photoevaporation flows leading to mass-loss rates of the order of 10 -7 solar mass per year or more, in good agreement with earlier spectroscopic observations of ionised gas tracers. Following this work, I developed a 1D hydrodynamical code to study the dynamical evolution of an externally illuminated protoplanetary disk. [...]

[pt] O tamponamento de poços de petróleo é analisado numericamente. Neste processo, um fluido mais denso (pasta de cimento) é colocado sobre outro menos denso (fluido de perfuração) em um poço vertical, resultando em uma situação de instabilidade. O escoamento resultante foi estudado de forma a avaliar se o isolamento do poço ocorreria até o momento da cura do cimento (entre 4 e 5 horas). O cimento foi modelado como fluido não-newtoniano e o fluido de perfuração foi considerado newtoniano em alguns casos e não-newtoniano nos demais casos. A solução do escoamento foi obtida numericamente, usando-se o programa ANSYS Fluent. As equações de conservação são resolvidas empregando-se o Método dos Volumes Finitos e o escoamento multifásico foi modelado utilizando-se o método Volume de Fluido. O comportamento viscoplástico não-newtoniano foi modelado empregando a equação constitutiva do fluido newtoniano generalizado, com a função de viscosidade Herschel-Bulkley. O sucesso da operação foi determinado pela combinação dos parâmetros reológicos e geométricos. O efeito dos parâmetros como a razão entre densidades e viscosidades foi investigado para uma geometria fixa (razão fixa entre o comprimento do tampão e o seu diâmetro). Além disso, a influência dessa mesma razão no processo também foi analisada enquanto outros parâmetros foram mantidos fixos. Foi demonstrado que o escoamento é muito instável e que os parâmetros estudados afetam consideravelmente a operação. / [en] The plugging process of an oil well was analyzed numerically. In this process, the denser fluid is the cement plug, which was placed above the drilling fluid in a vertical well, resulting in an unstable situation. The cement plug was modeled as non-Newtonian and the drilling fluid was considered Newtonian in some cases and non-Newtonian in other cases. The flow solution is studied using the ANSYS Fluent program. The conservation equations were solved using the Finite Volume Method, and the multiphase flow was modeled with the Volume of Fluid method. The non-Newtonian viscoplastic behavior of the cement plug was modeled with the Generalized Newtonian Fluid constitutive equation, with the Herschel-Bulkley viscosity function. The success of the operation was determined by the combination of the governing rheological and geometric parameters. The effect of the governing parameters, such as the density ratio and the viscosity ratio, were investigated for a fixed geometry and a fixed ratio between the cement plug length and diameter. Furthermore, the influence of this ratio in the process was also analyzed while others governing parameters were fixed. It was shown that the flow is highly unstable, and that the governing parameters considerably affect the operation.

Made available in DSpace on 2014-06-11T19:23:39Z (GMT). No. of bitstreams: 0 Previous issue date: 2006-12-18Bitstream added on 2014-06-13T18:10:05Z : No. of bitstreams: 1 kiryu_hs_me_ilha.pdf: 2419349 bytes, checksum: 258056fdacb79f386b2e6b238dc26028 (MD5) / Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) / Esta dissertação de mestrado traz à discussão o comportamento reológico de misturas formadas por água+colóides+detritos (areia fina), visando entender e esclarecer os processos físicos e mecânicos, tais como sedimentação e ressuspensão de materiais inertes no seio da massa fluida não-newtoniana (água+colóides), bem como verificar a validade ou adeqüabilidade do modelo reológico de Herschel-Bulkley (modelo previamente investigado e validado para misturas compostas de água+colóides) para misturas viscoplásticas com presença de grãos. A variação das propriedades reológicas das misturas, em função das características físicas dos grãos (diâmetro, massa específica e área superficial), é investigada, e um modelo de estimativa de tensão crítica é apresentado. Ademais foram realizados ensaios preliminares de escoamento de fluidos hiperconcentrados em canais inclinados, na tentativa de calibrar uma lei de atrito. Dentro dessas perspectivas, a dissertação é composta de 6 Capítulos com um denso Estado da Arte que descreve os fenômenos e mecanismos que regem os escoamentos desse tipo de compósito. Com base na literatura estudada e, a partir da análise dos resultados experimentais, pôde-se concluir que, para misturas compostas de água+colóides+detritos, o comportamento reológico das misturas é o mesmo que aquele do fluido intersticial (água+colóides), desde que a homogeneidade da mistura seja garantida (não ocorrência de sedimentação e ressuspensão sucessivas). Neste caso, o modelo reológico de Herschel-Bulkley continua sendo válido para explicar as curvas de escoamento ou de fluxo das misturas viscoplásticas com grãos. Para misturas que apresentem os fenômenos de sedimentação e ressuspensão, o modelo de Bagnold, adaptado a fluidos hiperconcentrados... / This work retakes the discussion about the rheological behavior of mixtures composed by water+ kaolinitic clay+fine sand in order to investigate the physical and mechanical processes such as sedimentation and suspension of inert materials into the non-Newtonian or interstitial fluid (water+colloids), as well as verify the adaptability of the Herschel-Bulkley rheological model (model previously investigated and validated for composed mixtures of water+ kaolinitic clay) for explain the viscoplastic+coarse materials rheological properties. The variation of the rheological properties of the mixtures in function of the coarse material characteristics (diameter, specific mass and superficial area) was investigated and a model predicting yield stress was proposed. Furthermore, some tests were performed in an inclined canal to determine a friction law for this kind of fluids. Inside of these perspectives, this dissertation is composed of 6 Chapters whit a dense State of the Art describing the phenomena and their mechanisms were pointed up. Based on literature and from the experimental results, one could concluded that the viscoplastic + coarse material mixtures behavior is the same of the interstitial fluid one, since that the homogeneity of the mixture is guaranteed (not occurrence of successive sedimentation and resuspension). In this case, Herschel-Bulkley rheological model is still valid to explain the curves of flow of the viscoplastic + coarse material. For mixtures that present the phenomena of sedimentation and resuspension, Bagnoldþs model, adapted to the hyperconcentrated fluids, describes well the variations of rheological parameters in function of the shear rates applied. Finally, it could be concluded that the experiments of free surface in canals, despite partial, can... (Complete abstract click electronic access below)

Une fraction non négligeable de l'histoire de la formation stellaire a lieu dans des environnements très affectés par la poussière. Il est donc naturel de se demander si on arrive à bien contraindre cette activité de formation d'étoiles. En effet, une part importante de cette activité pourrait être manquée due à la présence de poussière. C'est dans ce contexte que s'inscrit le travail que je vais présenter.Dans la première partie de ma thèse, j'ai eu pour but de déterminer la fraction de galaxies lumineuses formant des étoiles à haut redshift (i.e. 1.5<z<3) sélectionnées à partir des observations MIPS-24μm du champs COSMOS manquées par les critères UV/optique que je détaille ci-après. J'ai appliqué à mon échantillon de galaxies les critères BzK et BM/BX, ainsi que la sélection des «IRAC peakers» et celle des sources optiquement faibles mais brillantes en IR (OFIR, de l'anglais «Optically Faint IR-bright sources»). J'ai ensuite quantifié la contribution de ces différentes sous-populations à la fonction de luminosité à 8μm au repos ainsi qu'à la densité de taux de formation d'étoiles à z~2. Les résultats obtenus soulignent le danger d'utiliser des sélections couleurs de ce type lorsque l'on cherche à quantifier la formation stellaire enfouie dans la poussière. En effet, si le critère BzK offre une identification quasi-complète (~90%) de l'échantillon 24μm, il n'en est pas de même des autres critères. Par exemple, la sélection BM/BX manque 50% des sources considérées et celle des «IRAC peakers» ne sélectionne que 64% de l'échantillon d'étude. Il faut par conséquent être prudent lorsqu'on décide d'utiliser de telles méthodes de sélection qui entraînent nécessairement des extrapolations incertaines, pouvant ainsi fausser notre compréhension de la contribution des galaxies fortement affectées par l'extinction.Dans une seconde partie, je cherche à comprendre la nature composite des sources OFIR les plus brillantes. Cette démarche vise à apporter une compréhension supplémentaire à la connexion AGN/galaxie à flambée de formation stellaire. En se basant sur les données PACS à 100 et 160 μm du satellite herschel, je peux mieux contraindre les distributions spectrales d'énergie de mes sources. Je souhaite déterminer la fraction de la luminosité de ces sources due à la présence d'un AGN ou à la forte activité de formation stellaire dans le but de mieux comprendre le lien entre ces deux phénomènes. Ces sources OFIR brillantes (F_24μm> 1mJy) présentent des couleurs 100/24 et 160/24 plus faibles que les autres sources du champ COSMOS et leur luminosité semble donc provenir majoritairement d'un AGN. Les avancées technologiques et l'exploration des longueurs d'ondes en infra-rouge lointain et en submillimétrique, avec notamment Herschel, SCUBA-2, Alma, JWST, permettront de mieux comprendre la connexion AGN/ flambée de formation stellaire au sein des galaxies jusqu'à des hauts redshifts. / A non-negligible fraction of the star formation across cosmic time occurred within dust-enshrouded environment. One question of the main interest is then do we really know the exact amount of star formation activity. Indeed, this amount could be strongly biased by the effect of dust extinction.This features the context of the work I will discuss here.First of all, I focused my work on determining the number of luminous star-forming galaxies at 1.5<z<3 that are potentially missed by traditional UV/optical selections. I based my work on 24μm sources brighter than 80μJy in the COSMOS field. I applied to this mid-IR selected sample the BzK and BM/BX criteria, as well as the selections of the "IRAC Peakers" and the "Optically Faint-IR bright" galaxies (OFIR). I also quantified the contribution of these sub-populations to the IR luminosity and cosmic star formation density at z~2. I found that the BzK criterion offers an almost complete (~90%) identification of the 24μm sources at 1.4<z<2.5. In contrast, the BM/BX criterion misses 50% of the MIPS sources and the "IRAC Peakers" one only selects 64% of my sample. Color selections of distant star-forming galaxies must be indeed used with a lot of caution given the substantial bias they can suffer. In particular, the effect of dust extinction strongly affects the completeness of identifications at the bright end of the bolometric luminosity function, which could lead to large and uncertain extrapolations in order to account for the contribution of dusty galaxies missed by these selections.In a second time, I was interested in the composite nature of ultra-luminous infra-red galaxies presenting extreme optical/mid-IR colors at z∼2. I here try to better understand the Starburst/AGN connection in the brightest sources of my OFIR sample. Using PACS 100 and 160 μm from the Herschel Telescope, I have better constraints on the spectral energy distributions of the sources. The goal here is to determine the fraction of the IR luminosity due to the AGN and the fraction due to a strong star-forming activity. Theses really bright (F_24μm> 1mJy) OFIR sources present fainter 100/24 and 160/24 colors than the rest of the 24μm-selected sources. Their luminosity might then come from a strong AGN activity. The forthcoming facilities that will operate at long wavelengths (e.g., JWST, AKMA, SCUBA-2, etc.) will allow a better understanding of the link between the AGN activity and the star-forming one, up to high redshifts.

É notório que a degradação ambiental vem ao longo do tempo posicionando-se como um dos principais problemas do mundo moderno. Dentre as várias questões do interesse ambiental podemos destacar a ascensão da bolha de metano, em reservatórios hidrelétricos, desde o sedimento anóxico no fundo do reservatório até a interface água atmosfera. Neste contexto, a presente tese vêm propor uma nova modelagem matemática para a ascensão da bolha axissimétrica em fluidos newtonianos/nãonewtonianos e mostrar resultados numéricos simulados. Desta forma, o estado da arte estaria elevado a posição de permitir, via Matemática e Simulação Numérica-Computacional, a análise do transporte de metano em reservatórios de hidrelétricas através da bolha / It is well-known that environmental degradation has come along the time positioning as one of the main problems from modern world. Among several questions of the environmental interest may emphasize the methane bubble rise in hydroelectric reservoirs from the anoxic sediment in the bottom of reservoir until water interface atmosphere. In this context, the current thesis has come to propose a new mathematic modeling to the rise of the axisymmetric bubble in the newtonian/non-newtonian fluids and display numerical results simulated. Therefore, the state of art would be ascended to a position to permit, via Mathematics and Computing-Numeric Simulation, the analysis of transport of methane in hydroelectric reservoirs through of bubble

Massive star formation takes place in the dense cores of molecular clouds where the stars may be obscured at optical wavelengths. An excellent signpost of a massive young stellar object is the presence of an ultra-compact HII region (UCHii), which is a dense photo-ionised cocoon of gas surrounding the newly formed star. The aim of this project is to develop an assembly of numerical tools, caravela, that can simulate realistic data streams representing high-mass star forming regions in our Galaxy. The synthetic output consists in images and photometric point source catalogues, in the IRAS and Herschel wavebands. In an era when large observational surveys are increasingly important, this tool can produce simulated infrared point-source catalogues of high-mass star forming regions on a Galactic scale. The approach used is to construct a synthetic Galaxy of star-forming regions represented by SED templates. The star-forming regions are distributed randomly along a four spiral arm morphology, although a wide range of geometries can be used including rings and different numbers of spiral arms. The caravela code then observes the synthetic Galaxy to produce simulated images and point source catalogues with appropriate sensitivity and angular resolution. caravela was first used to model the simulated Galaxy by constraining the synthetic output to observations made by IRAS. This numerical tool will allow the user to infer physical properties of the Galactic population of high-mass star forming regions from such observations. Second, the selected model was again observed with caravela in Herschel mode. These are therefore predictive results for the future Herschel observations. A model with 4.0×104 compact proto-stars embedded in larger grey-body envelopes (with T = 40 K and linear size scale lIII = 5.0 × 106 AU) is the best-fit model to the IRAS observational data set studied. We found a level of contamination from low- and intermediate-mass objects of " 90%. The modelled data set resulting from the Herschel simulation resulted in the detection of approximately twice as many Herschel objects than IRAS, which is consistent, in a limited way, with the real observed companion clump fraction (CCF) of 0.90 ± 0.07 (Thompson et al., 2006) means that on average there were observed 2 sources per one IRAS source. Our caravela and the real observed CCF are therefore consistent. caravela was coupled with an independent diffuse emission model (Paladini et al., 2007) and the resulting analysis is presented as an interesting seed for the future.