Made available in DSpace on 2014-06-11T19:23:39Z (GMT). No. of bitstreams: 0 Previous issue date: 2007-11-21Bitstream added on 2014-06-13T20:50:45Z : No. of bitstreams: 1 ferreira_fo_me_ilha.pdf: 819769 bytes, checksum: 88d8eb791de97678aeffb0163237a264 (MD5) / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / Os escoamentos em superfície livre que ocorrem em canais inclinados, tanto em fluido Newtoniano quanto em fluido não-Newtoniano (hiperconcentrado), podem desenvolver instabilidades, tais como ondas em forma de ressalto hidráulico, com comprimentos bem definidos. Tais perturbações são denominadas Roll Waves. Essas ondas são comuns em canais artificiais, em lavas torrenciais e deslizamento de avalanchas. Neste trabalho, no plano teórico, é determinado um modelo matemático geral, com base nas equações de Navier- Stokes integradas na vertical, em cujo tensor de tensões é introduzido a reologia de Herschel- Bulkley. A velocidade média do escoamento é determinada levando-se em consideração que o escoamento apresenta um perfil de velocidade parabólico na região cisalhada (próximo ao fundo do canal) acoplado a um perfil linear na região não cisalhada (condição de plug), característico dos escoamentos de lamas e detritos. A partir do sistema de equações (conservação da massa e equação da quantidade de movimento) em variáveis adimensionais, uma análise de estabilidade linear é realizada, colocando em evidência as condições de formação dessas instabilidades, tanto em fluido hiperconcentrado como em fluido Newtoniano. Com as condições de formação de instabilidades estabelecidas, uma teoria analítica de Roll Waves permanente é imposta e um modelo matemático para geração de tais instabilidades é determinado. No plano numérico, utilizando a linguagem de programação Python, a validade do modelo é verificada, considerando que essas ondas são ajustadas por choques devido às singularidades existentes no modelo. Com a determinação das condições de choque e da velocidade de propagação da onda em um ponto crítico; pode-se observar a formação de Roll Waves em fluidos não Newtonianos com reologia de Herschel-Bulkley, Bingham, Power Law, como também em fluido Newtoniano. / The flows in free surface that occur in sloping canals, such as Newtonian fluid as in non- Newtonian fluid (hyperconcentrated), they can develop instabilities, such as long waves in form of hydraulical jumps, with well defined lengths; these instabilities are called Roll Waves, more common in artificial canals, torrential spillways of dams, lava and avalanche landslide. This work, in the theoretical plan, a general mathematical model is determined, on the basis of the integrated Navier-Stokes equation in the vertical, of tensor tensions the rheology of Herschel-Bulkley is introduced. The average velocity of the flows is determined taking itself in consideration that the flows presents a parabolic profile of speed in the shear region (near of the floor of canal) connected to a linear profile in the region not shear (condition of plug), categorized as flows of mudflows and debris flows. From the system of equations (conservation of the mass and equation of the momentum) in adimensional variables, an analysis of linear stability is carried through, placing the conditions of formation of these instabilities, as much in hyperconcentrated fluid as in Newtonian fluid. With the conditions of formation of instabilities established, a analytical theory of permanent Roll Waves is imployed and a mathematical model for geration of such stabilities it’s determined. In the numerical plan, using the computational consol Python, the validity of model is checked, considering of this waves are adjusted by shocks devided by the singularities existents in the model. With the determination of conditions of shock and the velocity of propagation of wave in a critical point; we can observe the formation of Roll Waves such in fluids non-Newtonians (Herschel- Bulkley, Bingham, Power law) as Newtonian fluids.

The most intensely star-forming galaxies lie at z ∼ 2 and are thought to be the progenitors of the most massive galaxies today, yet study of this important population has been hampered by vast quantities of dust, making them almost invisible in the optical and ultraviolet (UV) regimes, and by the low sensitivity and angular resolution of many infrared (IR) facilities. Chapter 2 describes the use of the flux and angular extent boost provided by strong gravitational lensing in the detailed study of individual high-redshift dusty star-forming galaxies (DSFGs). The low number density of such systems has been overcome by recent wide area far-infrared (FIR)–mm surveys, and a sample of candidate systems which are bright enough to study with single-dish FIR telescopes are assembled from these surveys. The chapter further describes spectra of these galaxies obtained using the the Spectral and Photometric Imaging REceiver (SPIRE; Griffin et al. 2010) Fourier transform spectrometer (FTS) on board the Herschel Space Observatory (Pilbratt et al. 2010), exploiting the increased flux densities to search for FIR atomic and ionic spectral lines: important coolants of warm gas surrounding star-formation regions. Chapter 3 describes the first “blind” redshift obtained using Herschel, via the detection of [C ii] 158 μm in one of our spectra. Confirmation of this redshift was provided by detection of CO lines with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) and the Plateau de Bure Interferometer (PdBI), and along with multi-wavelength photometric follow-up, allowed a characterisation of the galaxy, indicating both a merger-driven starburst and an active galactic nucleus (AGN) within the system. Chapter 4 describes the first detection of a massive outflow of molecular gas at high-redshift. Stacking five repeat spectra of the Cosmic Eyelash, one of the best-studied strongly lensed DSFGs, one of the massive star-forming clumps is shown to drive this outflow, albeit likely at a velocity lower than that required to become unbound from the hosting gravitational potential well. Chapter 5 describes line measurements and spectral energy distribution (SED) fitting from the full set of spectra and Herschel PACS mini scan maps. The spectra are stacked to search for faint lines, and compared to a detailed interstellar medium (ISM) model to determine average physical properties of the star-forming gas. Photodissociation region (PDR) properties are found to be similar to those derived using other models, however a cosmic ray ionisation rate of 103 times that of the Milky Way, expected in galaxies of this type cannot reproduce the observed line ratios, in particular the low [O i] 63 μm flux. Chapter 6 finally describes the conclusions drawn from the work presented in this thesis and how these data and analysis add to our knowledge and interpretation of high-redshift DSFGs.

The application of the Hershcel-Quincke (HQ) tube as a noise reduction device for one-dimensional plane-wave sound fields has been studied in great detail in previous years. In this thesis, an analytical technique is developed to investigate the potential of the HQ tube concept to control higher-order duct modes. This analytical method involves modeling the tube-duct interfaces as finite piston sources, which couple the acoustic field inside the main duct with the acoustic field within the HQ tube(s). The acoustic field within the HQ tube is modeled as plane-waves and the acoustic field within the main duct is modeled by expanding the sound field in terms of the higher-order modes. This model is then used to investigate the noise reduction mechanisms behind the attenuation of higher-order modes. These mechanisms involve both the reflection of the incident wave as well as the reconstruction and recombination of the modal content of the incident disturbance into other modes. The effects of the modal content of the disturbance along with the HQ tube geometric parameters, such as tube axial position, length, distance between interfaces, and cross-sectional area, are studied with respect to the frequencies of attenuation and the reduction obtained. These results show the potential of the Herschel-Quincke tube concept to reduce higher-order modes in ducts. / Master of Science

Drilling is crucial to many industries, including hydrocarbon extraction, CO2 sequestration, geothermal energy, and others. During penetrating the subsurface rocks, drilling fluid (mud) is used for drilling bit cooling, lubrication, removing rock cuttings, and providing wellbore mechanical stability. Significant mud loss from the wellbore into the surrounding formation causes fluid lost-circulation incidents. This phenomenon leads to cost overrun, environmental pollution, delays project time and causes safety issues. Although lost-circulation exacerbates wellbore conditions, prediction of the characteristics of subsurface formations can be obtained. Generally, four formation types cause lost-circulation: natural fractures, and induced fractures, vugs and caves, and porous/permeable medium. The focus in this work is on naturally fractured formations, which is the most common cause of lost circulation. In this work, a novel prediction tool is developed based on analytical solutions and type-curves (TC). Type-curves are derived from the Cauchy equation of motion and mass conservation for non-Newtonian fluid model, corresponding to Herschel-Bulkley model (HB). Experimental setup from literature mimicking a deformed fracture supports the establishment of the tool. Upscaling the model of a natural fracture at subsurface conditions is implemented into the equations to achieve a group of mud type-curves (MTC) alongside another set of derivative-based mud type-curves (DMTC). The developed approach is verified with numerical simulations. Further, verification is performed with other analytical solutions. This proposed tool serves various functionalities; It predicts the volume loss as a function of time, based on wellbore operating conditions. The time-dependent fluid loss penetration from the wellbore into the surrounding formation can be computed. Additionally, the hydraulic aperture of the fracture in the surrounding formation can be estimated. Due to the non-Newtonian behavior of the drilling mud, the tool can be used to assess the fluid loss stopping time. Validation of the tool is performed by using actual field datasets and published experimental measurements. Machine-Learning is finally investigated as a complementary approach to determine the flow behavior of mud loss and the corresponding fracture properties.

No description available.

<p>The study of ongoing mergers is vital to understanding how intense star bursts are triggered, and how luminous infrared galaxies and ultra luminous infrared galaxies are formed. The Antennae (NGC 4038/39), at a distance of only 24.9 Mpc, represents the nearest example of a major merger between two gas rich spirals and provides us with a unique laboratory for studying molecular gas and star formation. I have obtained two fully sampled observations of the Antennae using the Herschel SPIRE Fourier Transform Spectrometer which I have supplemented with JCMT CO J = 3 − 2 observations. I detect CO, CI and NII emission throughout both the overlap region and the nucleus of NGC 4038. I measured the integrated intensity of the CO J = 4−3 to 8−7 and find that the overlap region is brighter for all but the J = 4 − 3 line. I find that, in the nucleus of NGC 4038, the CO spectral line energy distribution peaks at the 4−3 transition, while in the overlap region it peaks at the 3−2 transition. I modelled the CO emission using the non-local thermal equilibrium radiative transfer code RADEX coupled with a Bayesian likelihood code. I find a warm (Tkin > 600K) lower density (nH2 ∼ 200cm−3) component of molecular gas in the nucleus of NGC 4038, and similarly in the overlap region (Tkin > 600 K, nH2 ∼ 300cm−3) and find widespread evidence for multiple components of molecular gas throughout the system. These warm components in both regions correspond to ~ 1% of the total molecular gas. I find no evidence of x-ray dominated regions, cosmic rays or turbulent heating being the primary source of heating throughout the galaxy, while photodissociation regions or supernova and stellar winds may be the primary source of heating throughout the galaxy.</p> / Master of Science (MSc)

Studiens syfte är att undersöka potentialen och effektiviteten av spiralljuddämpare jämfört med standardljuddämpare för kompressorer i Värme och luftkonditionerings system i bilar. Den ökande efterfrågan på kompakta och effektiva lösningar inom fordonsindustrin, ledde till utforskning av alternativa tekniker som kan bidra till att förbättra bilens prestanda och passagerarkomfort. En ljuddämpartyp som vore intressant att nyttja för denna tillämpning är spiralformade ljuddämpare. Dessa enheter är mer kompakta jämfört med standardljuddämpare, vilket gör dem till ett attraktivt alternativ för biltillverkare som strävar efter att optimera utrymmesanvändningen inom fordonet. Dessutom, tidigare studier visade att spiralformade ljuddämpare kan erbjuda effektiv akustisk dämpning, vilket kan bidra till en mer bekväm och tyst körupplevelse. I denna studie kommer vi att genomföra en omfattande litteraturöversikt över befintliga modeller och prestanda för spiralljuddämpare. Vi kommer sedan att genomföra en jämförande analys mellan spiralformade ljuddämpare och standardljuddämpare en s.k. expansionskammare. Resultaten från denna analys kommer att presenteras och diskuteras i detalj, med syftet att dra slutsatser om effektiviteten av spiralformade ljuddämpare och deras potential för framtida tillämpningar inom fordonsindustrin. Denna studie kommer att genomföras i samarbete med Volvo Cars i Göteborg.

Les domaines millimétrique et submillimétrique sont des domaines qui permettent de caractériser la physico-chimie des atmosphères planétaires par l'observation des molécules qui les composent. Le télescope spatial Herschel et l'interféromètre ALMA, qui entreront prochainement en service, permettront d'améliorer considérablement notre connaissance des atmosphères planétaires. L'un des principaux objectifs de cette thèse est de développer un modèle d'analyse des observations millimétriques et submillimétriques qui seront effectuées avec Herschel et ALMA. C'est en ce sens que nous détaillons un modèle qui tient compte de la géométrie sphérique des corps observés et des spécificités instrumentales propres aux télescopes utilisés. Dans un premier temps, ce qui a permis notamment de valider notre modèle de transfert radiatif, nous avons étudié l'origine des composés oxygénés dans les atmosphères des planètes géantes. Nous présentons l'analyse d'observations de Saturne et d'Uranus, effectuées avec les télescopes de l'IRAM et du JCMT, pour contraindre les sources de monoxyde de carbone dans ces atmosphères. Nous améliorons ainsi les limites supérieures précédemment publiées et réalisons la première observation du monoxyde de carbone dans l'atmosphère de Saturne dans le domaine submillimétrique. Cette observation prouve l'existence d'une source externe pour ce composé. Nous analysons également des observations récentes de Jupiter, effectuées par le télescope spatial Odin, pour contraindre l'origine externe de l'eau dans la stratosphère de cette planète. Les observations confirment que la chute de la comète Shoemaker-Levy~9 est vraisemblablement la source principale d'eau. Dans un second temps, nous avons appliqué notre modèle à l'étude de la structure thermique et la dynamique de l'atmosphère de Mars, à partir d'observations du monoxyde de carbone. Ces observations sont comparées aux prédictions d'un modèle de circulation générale, ce qui permet de vérifier la validité de ses prédictions et de fournir de nouvelles contraintes observationnelles pour ce type de modélisations. Enfin, nous avons appliqué notre modèle à l'étude des planètes géantes avec le télescope spatial Herschel, dans le cadre du programme-clé de temps garanti du télescope spatial Herschel ``Water and related chemistry in the Solar System''. Nous avons également identifié les améliorations à apporter à notre modèle pour analyser des observations ALMA. / The planetary atmospheres can be characterized by observations carried out in the millimeter and submillimeter wavelength ranges. In a near future, the Herschel Space Observatory as well as the ALMA interferometer will increase our knowledge of the planet atmospheres. One of the main goals of this thesis work consists in developping an analysis tool for millimeter and submillimeter observations, which will be carried out with Herschel and ALMA. The model we have developped takes into account the spherical geometry of the planets and the properties of the telescopes. First, we have studied the origin of oxygen compounds in the atmospheres of the giant planets. We have validated our radiative transfer model from this study. We present the analysis of observations of carbon monoxide in the atmospheres of Saturn and Uranus, which have been carried out with the IRAM and JCMT telescopes, in order to constrain the origin of this compound. We improve existing upper limits and prove the existence of an external source of carbon monoxide in the atmosphere of Saturn from the first observation of this compound at submillimeter wavelengths. We also analyse recent observations from the Odin space telescope of water vapor in the stratosphere of Jupiter to constrain its external source. We confirm that the observed water is probably mostly due to the collision of comet Shoemaker-Levy~9 with the planet. Then, we have used our model in order to study the thermal structure as well as the dynamics of the atmosphere of Mars from carbon monoxide observations. These observations are compared to predictions of a general circulation model to check the consistency of the predictions. They also provide new observational constraints to general circulation models. Finally, we have used our model to study the atmospheres of the giant planets in the frame of the Herschel garanteed time key-program ``Water and related chemistry in the Solar System''. We have also determined the upgrades to implement in our model to analyse ALMA observational data.

Les radio galaxies sont les candidats préférentiels pour comprendre la formation et l'évolution des galaxies sur une grande échelle de temps. Observées jusqu'à z>5 en raison de leur brillance, elles sont abritées par des galaxies elliptiques géantes. L'émission radio révèle la présence d'un trou noir supermassif. Un tore de poussière entourant le noyau actif de galaxie (AGN) agit comme un coronographe naturel permettant alors l'étude de la galaxie hôte. L'objectif de cette thèse est de déterminer l'évolution de la composante stellaire en présence d'un AGN. La décomposition est faite à partir de la distribution spectrale d'énergie (SED) de l'UV au submillimétrique en utilisant le code d'évolution de galaxies PEGASE.3 et un code d' AGN, les deux modélisant l'émission de la poussière par transfert radiatif.En premier lieu, nous présentons le projet HeRGE, 70 radio galaxies observées avec Herschel, qui permet de mesurer leurs luminosités totales infrarouges, comparables à celles des ULIRG. Une décomposition de la luminosité infrarouge entre l'émission AGN et un modèle de starburst est proposée pour l'ensemble de l'échantillon. Ces luminosités élevées sont interprétées en termes de taux d'accrétion et de formation d'étoiles, favorisant la croissance du trou noir par rapport à la galaxie hôte.En second lieu, l'orientation du jet par rapport au tore est contrainte à partir de l'infrarouge moyen et du rapport des émissions radio des lobes (isotrope, 500MHz) et du coeur (anisotrope, 20GHz). Ces observations en accord avec le modèle d'unification permettent d'évaluer le facteur d'absorption Av, l'inclinaison du tore et de contraindre le facteur de Lorentz.Une sélection de 12 radio galaxies observées de l'UV au sub-mm est analysée avec PEGASE.3 et un modèle d'AGN. Une seule composante stellaire est insuffisante. Seules deux composantes (une évoluée et massive, et une jeune issue d'un starburst) permettent un ajustement significatif de la SED complète. La composante évoluée est très massive (environ 10^12 msun) formée sur une courte période de temps (<10^9 ans). La composante jeune (<4.10^7 ans), moins massive (environ 10^11 msun), confirme un processus épisodique de croissance par sursauts. Ces résultats sont des contraintes fortes pour les modèles de formation de galaxies. La relation avec le noyau actif reste encore à préciser. Les projets d'observations complémentaires, optique et mm, permettront de confirmer ces résultats. / Powerful radio galaxies are excellent candidates for investigating and ultimately understanding the formation and evolution of galaxies. These beacons are now observed out to z>5 and are commonly associated with the massive early-type galaxies observed in the local universe. While the radio emission reveals the presence of a supermassive black hole, a dusty parsec-scale torus acts like a natural coronograph, making it easier to study the properties of the host galaxy. The aim of this PhD thesis is to characterise the nature and evolution of the stellar population and the relationship between the stellar population and the active galactic nucleus (AGN). To reach our scientific goals, we use the galaxy evolution code, PEGASE, combined with a AGN model which both consider the radiative transfer of the UV, optical, and IR photons through dust. To begin, we present the HeRGE project consisting of 70 radio galaxies which have been observed with Herschel. These IR observations allow us to calculate the total infrared luminosities and reveal that our sample belongs to the ULIRG regime. We decompose the infrared SED into an AGN and starburst components using observational templates. Converted into accretion and star formation rate, their relative luminosities indicate that the black holes are growing proportionally faster than are the host galaxies.In addition, we constrain the configuration of the jet and torus by combining the results from mid-infrared spectral energy distribution (SED), and the radio emission from the lobes (isotropic at 500MHz) and the core (anisotropic at 20GHz). In agreement with the unified scheme, these observations allow us to estimate the absorption Av, the inclination of the torus, and provides a constraint on the Lorentz factor for the radio jet.A subsample of 12 radio galaxies observed from the UV to sub-mm is also analysed with PEGASE.3 and an AGN torus model. While one stellar component is clearly insufficient to fit the observations, two stellar components are necessary to successfully reproduce the SED (one evolved and massive, about 10^12 msun, formed over a reasonably short time, <1Gyr at high redshift; and a much younger component, <40Myr, that is also less massive, about 10^11 msun. Such a star formation history suggests rapid growth at high redshift of longer duration followed much by another period of rapid, stochastic growth.These results put strong constraints on galaxy formation models. Unfortunately, the crudeness of some of our data and theoretical understanding the IR emission from AGN, means that the relation of the galaxy to its AGN is still not well constrained. Additional observations at optical through millimeter wavelengths are needed to extend our findings.

Cette thèse présente une étude expérimentale visant à caractériser les propriétés hydrauliquesd'écoulements à surface libre de fluides complexes: fluides viscoplastiques et mélangesfluides viscoplastiques-grains. Ce travail est motivé par la nécessité d'améliorer lesconnaissances sur les propriétés des écoulements de laves torrentielles, dans un contexte deprotection contre les risques naturels en montagne. Nous avons développé un dispositif delaboratoire original, un canal à fond mobile, permettant de générer des coulées gravitaires quisont globalement stationnaires dans le référentiel du laboratoire. Les coulées présentent unfront très raide, suivi à l'amont d'une zone d'épaisseur uniforme. Les fluides viscoplastiquesutilisés (carbopol et kaolin) ont été choisis de manière à modéliser la matrice des couléesboueuses naturelles en prenant en compte les critères de similitude adaptés. Ces fluidessuivent une loi de comportement de Herschel-Bulkley, et leurs propriétés rhéologiques ont étédéterminées au moyen d'un rhéomètre de laboratoire en accordant un soin particulier àl'établissement des incertitudes associées. Nous présentons des mesures précises de l'évolutionde l'épaisseur des coulées dans la zone uniforme en fonction de la vitesse du fond du canal etde la pente. Ces résultats sont comparés à des prédictions théoriques correspondant à unécoulement permanent et uniforme d'un fluide de Herschel-Bulkley, et nous montrons quel'accord est satisfaisant moyennant les incertitudes sur les mesures rhéologiques. Nous avonségalement analysé la forme du front des coulées et, là-aussi, l'accord avec des modèleshydrauliques (modèles de type Saint-Venant) est bon. Ces deux études permettent de validerles prédictions hydrauliques obtenues à partir de lois de comportement mesurées aurhéomètre. Enfin, dans une dernière partie, nous présentons une étude préliminaire de ladynamique de particules rigides isolées placées au sein de la coulée, en nous intéressant auxvitesses longitudinales et aux vitesses de chute pour différentes tailles et différentes densitésde particules. / This thesis presents an experimental study dedicated to characterise the hydraulic propertiesof free surface flows of complex fluids : viscoplastic fluids and mixtures made of viscoplasticfluids and grains. This study is motivated by the need to improve knowledge on properties ofthe flow of debris flows in a context of protection against natural hazards in the mountains.We have developed an original laboratory device - a channel with a mobile bottom - togenerate gravitary flows that are globally stationary in the laboratory frame. The flows have avery steep front followed upstream by a zone of uniform thickness. Viscoplastic fluids used(carbopol and kaolin) were selected so to model the matrix of natural mud flows, taking intoaccount the criteria of similarity adapted. These fluids follow a behavior law of Herschel-Bulkley, and their rheological properties were determined using a laboratory rheometer byproviding a particular care to the establishment of the associated uncertainties. We presentaccurate measurements of the evolution of the thickness of the flow in the uniform zone withthe the velocity speed of channel belt. These results are compared with theoretical predictionscorresponding to a steady uniform flow of a fluid of Herschel-Bulkley, and we show that theagreement is satisfactory through the uncertainties on the rheological measurements. We alsoanalyzed the shape of front, and here too, the agreement with hydraulic models (models likeSaint-Venant) is good. Both of the studies allowed to validate the hydraulic predictionsobtained from behavior laws measured with the rheometer. Finally, in a last section, wepresent a Preliminary study about the dynamics of isolated rigid particles placed in the flow,by paying attention to longitudinal velocities and falling velocities for different particle sizesand densities.