För att ta byggbranschen till nästa steg i utvecklingen är BIM det naturliga steget. Iteorin tycks många av lösningarna som medföljer implementationen av BIM varaenkla att förstå och skapa, i praktiken ligger dock de tekniska lösningarna långt ifrånen full implementation i branschen. I arbetet med olika typer av beskrivningar inomett byggprojekt har utvecklingen med hjälp av BIM stått still länge. Då det inte finnsnågot vedertaget sätt att utnyttja en BIM-modells information för att fylla olikabeskrivningar måste det problemet lösas om en effektivisering ska kunna uppnås.Rapporten ämnar till att skapa ett arbetssätt för projektörer och personer inblandadei olika byggprojekt att hantera beskrivningar av utrymmen och information på ettenklare vis. Genom en analys av vilken information som är väsentlig för olikabeskrivningar har information exporterats ur och importerats tillbaka till en modell iAutodesk Revit, samt fördelats till rumsbeskrivningar. Med hjälp av modellen och denvisuella programmering som upprättats i Dynamo dras slutsatser att som systemetmed beskrivningar fungerar idag, är ett ineffektivt arbetssätt som kräver en tekniskupprustning. Mycket av informationen som upprättas i beskrivningarna finns att tillgåi Revitmodellen, men idag är den för det mesta outnyttjad och kvar i modellen varförett arbetssätt för att effektivisera detta presenteras. / To be able to take the construction industry to the next stage of development, thenatural step is by integrating BIM. In theory, it seems like many of the solutions thatcomes with the implementation of BIM are simple to understand and develop. Inpractice, however, the technical solutions are far from being completely implementedin the industry. In the making of different types of descriptions within a constructionproject, the development and progress using BIM has been idle for a long time. Asthere is no general way to utilize a BIM model's data to fill various descriptions, oneproblem to be resolved is the efficiency of the way the data is being handled. The reportintends to create a work flow for people involved in various construction projects todeal with descriptions of rooms and information in a more efficient way. Through ananalysis of which information that is essential for the different types of descriptions,information is being exported from and imported back to an Autodesk Revit model.The data is then distributed to room descriptions. With the help of the model and thevisual programming using Dynamo, conclusions are drawn that the way the systemwith descriptions works today is an inefficient way of working that requires a technicalupgrading. A lot of the information that is being established in the descriptions areavailable in the Revit model, but today it is mostly left unused and stuck in the modelas to why an approach to streamline this presented.

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Die Frage nach der Herkunft und der dynamischen Entwicklung langlebiger kosmischer Magnetfelder ist in vielen Details noch unbeantwortet. Es besteht zwar kein Zweifel daran, dass das Magnetfeld der Erde und anderer kosmischer Objekte durch den sogenannten Dynamoeffekt verursacht werden, der genaue Mechanismus als auch die notwendigen Voraussetzungen und Randbedingungen der zugrundeliegenden Strömungen sind aber weitgehend unbekannt. Die für einen Dynamo interessanten Strömungsmuster, die im Inneren von Himmelskörpern durch Konvektion und differentielle Rotation entstehen, sind Konvektionsrollen parallel zur Rotationsachse. Auf einer Strömung mit eben solcher Geometrie, der sogenannten Roberts-Strömung, basieren die in der vorliegenden Arbeit untersuchten Dynamomodelle. Mit Methoden der nichtlinearen Dynamik wird versucht, das Systemverhalten bei Änderung der Systemparamter genauer zu charakterisieren. Die numerischen Untersuchungen beginnen mit einer Analyse der Dynamoaktivität der Roberts-Strömung in Abhängigkeit von den zwei freien Parametern in den Modellgleichungen, der magnetischen Prandtl-Zahl und der Stärke des Energieinputs. Gefunden werden verschiedene Lösungstypen die von einem stationären Magnetfeld über periodische bis zu chaotischen Zuständen reichen. Die yugrundeliegenden Symmetrien werden beschrieben und die Bifurkationen, die zum Wechsel der Lösungstypen führen, charakterisiert. Zusätzlich gibt es Bereiche bei sehr kleinen Prandtl-Zahlen, in denen überhaupt kein Dynamo existiert. Dieses Verhalten wird in der Literatur auch für viele andere numerisch ausgewertete Modelle beschrieben. Im Übergangsbereich zwischen dynamoaktivem und dynamoinaktivem Bereich wird das Auftreten einer sogenannten Blowout-Bifurkation gefunden. Desweiteren beschäftigt sich die Arbeit mit der Frage, inwiefern Helizität, also eine schraubenförmige Bewegung, der Strömung den Dynamoeffekt beeinflusst. Dazu werden ähnliche Strömungstypen verglichen, die sich hauptsächlich in ihrem Helizitätswert unterscheiden. Es wird gefunden, dass ein bestimmter Wert der Helizität nicht unterschritten werden darf, um einen stabilen Roberts-Dynamo zu erhalten. / The question of origin and development of longlasting cosmic magnetic fields is in many details an unanswered question. There is no doubt that the magnetic fields of cosmic objects like the earth, the sun and larger structures are caused by the so called dynamo effect. The exact mechanism as well as the necassary properties and boundary conditions for the underlying flow field are mostly unknown. The flow pattern believed to act as the source of dynamo activity in the inner of cosmic bodies are convection-like rolls parallel to the rotation axis of this objects and are results of the acting body forces due to differential rotation and thermal convection. The basis of the considered dynamo model is a flow field revealing such flow structures, the so called Roberts flow. The numerical investigations start with an analysis of dynamo activity of the Roberts flow in dependence on the two free parameters magnetic Prandtl number and forcing strength. The model shows different types of solutions starting from steady magnetic states in a very small parameter region at larger magnetic Prandtl numbers, time-periodic solutions and chaotic behavior for stronger forcing. For small magnetic Prandtl numbers the system doesn't carry any magnetic field. This 'small Prandtl number problem' is in accordance with the behavior of several other numerically investigated dynamo models described in the literature. The transient region between dynamo activity and the non-magnetic states can be classified by a so-called blowout bifurcation. Furthermore the investigation deals with the question in what way the helical structure of the flow field indicated by a non-vanishing kinetic helicity influences the dynamo process. The comparison of very similar flow families, mainly distinguishable by their different helicity values, leads to the result that beneath a lower bound no stable Roberts dynamo is working.

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Convection in a Boussinesq fluid confined by a annular channel fast rotating about a vertical axis and uniformly heated from below, is one of our concerns in this thesis. An assumption that the channel has a sufficiently large radius in comparison with its gap-width is employed, so that the curvature effect can be neglected. The aspect ratio of the channel has great influence on the convective flow in it. Guided by the result of the linear stability analysis, we perform three-dimensional numerical simulations to investigate the convective flows under three different types of aspect ratios, which are namely the moderate or large aspect ratios, the very small aspect ratios and the moderately small aspect ratios. Also, we numerically study how convection in the channel is affected by inhomogeneous heat fluxes on sidewalls, which is a simple simulation of the thermal interaction between the Earth's core and mantle. Convection and dynamo action in a rapidly rotating, self-gravitating, Boussinesq fluid sphere is the other concern. We develop a finite element model for the dynamo problem in a whole sphere. This model is constructed by incorporating dynamo equations with globally implemented magnetic boundary conditions to a whole sphere convection model, which is also presented here. The coordinate singularity at the center usually encountered when applying the spectral method is no longer an obstacle and no nonphysical assumptions (i.e. hyper-diffusivities) are used in our model. A large effort has been made to efficiently parallelize the model. Consequently, it can take the full advantage of modern massively parallel computers. Based on this dynamo model, we investigate the dynamo process in a sphere and find that self-sustaining dynamos are more difficult to obtain in a sphere than in a spherical shell. They are activated at relatively high Rayleigh numbers. Moreover, the magnetic fields generated are not dipole-dominant, different from those generated in most dynamo simulations.

Sunspots and active regions are two of the many manifestations of the solar magnetic field. This field plays an important role in causing phenomena such as coronal mass ejections, flares, and coronal heating. Therefore, it is important to study the origin of sunspots and active regions and determine the underlying mechanism which creates them. It is believed that flux tubes rising from the bottom of the convection zone can create sunspots. However, there are still unanswered questions about this model. In particular, flux tubes are expected to expand as they rise, hence their strength weakens and some sort of reamplification mechanism must complement this model to match the observational properties of sunspots. To compensate for the absence of such an amplification mechanism, the field strength of the flux tubes, when at the bot- tom of the convection zone, must be far stronger than present dynamo models can explain. In the last few years, there has been significant progress toward a new model of magnetic field concentrations based on the negative effective mag- netic pressure instability (NEMPI) in a highly stratified turbulent plasma. NEMPI is a large-scale instability caused by a negative contribution to the total mean-field pressure due to the suppression of the total turbulent pressure by a large-scale magnetic field. In this thesis, I study for the first time NEMPI in the presence of a dynamo-generated magnetic field in both spherical and Carte- sian geometries. The results of mean-field simulations in spherical geometry show that NEMPI and the dynamo instability can act together at the same time such that we deal with a coupled system involving both NEMPI and dynamo effects simultaneously. I also consider a particular two-layer model which was previously found to lead to the formation of bipolar magnetic structures with super-equipartition strength in the presence of a dynamo-generated field. In this model, the turbulence is forced in the entire domain, but the forcing is made helical in the lower part of the domain, and non-helical in the upper part. The study of such a system in spherical geometry showed that, when the stratification is strong enough, intense bipolar regions form and, as time passes, they expand, merge and create giant structures. To understand the underlying mechanism of the formation of such intense, long-lived bipolar structures with a sharp boundary, we performed a systematic numerical study of this model in plane parallel geometry by varying the magnetic Reynolds number, the scale separation ratio, and Coriolis number. Finally, I investigate the formation of the current sheet between bipolar regions and reconnection of oppositely orientated magnetic field lines and demonstrate that for large Lundquist numbers, S, the reconnection rate is nearly independent of S – in agreement with recent studies in identical settings.

Chan Kit Hung. / "August 2002." / Thesis (Ph.D.)--Chinese University of Hong Kong, 2002. / Includes bibliographical references (p. 132-152). / Electronic reproduction. Hong Kong : Chinese University of Hong Kong, [2012] System requirements: Adobe Acrobat Reader. Available via World Wide Web. / Mode of access: World Wide Web. / Abstracts in English and Chinese.

Ce manuscrit est consacré à l'étude de trois aspects de la magnétohydrodynamique : l'effet dynamo, l'influence d'un écoulement turbulent de métal liquide sur un champ magnétique et l'influence d'un champ magnétique fort sur un écoulement turbulent de métal liquide. Des expériences en gallium à l'ENS-Lyon, et des expériences en sodium à Cadarache, au sein de la collaboration VKS (von Karman sodium), on été menées. Une partie est consacrée à l'importance des conditions aux limites pour les processus d'induction et les mécanismes dynamo, tels que révélés par l'expérience VKS. Nous présentons les résultats obtenus en modifiant la conductivité électrique et la perméabilité magnétique des disques dans l'expérience VKG (von Kármán gallium), à bas Rm. Ils mettent en évidence l'importance d'effets d'inductions forts au voisinage de disques en fer. De même, pour comprendre le lien entre la dynamique chaotique du champ dynamo dans l'expérience VKS et celle de l'écoulement turbulent, nous avons mis en place une expérience dynamo semi-homogène avec un effet ω turbulent et un bouclage artificiel. Le champ engendré par cette expérience présente une intermittence de type on-off pilotée par les grandes échelles de l'écoulement. Cette dynamique est alors analogue à celle d'un système avec bruit multiplicatif et bruit additif. Lors de la saturation du champ dynamo, la force de Laplace est suffisamment forte pour modifier l'écoulement et stopper la croissance du champ. Afin d'étudier ce phénomène, nous avons développé deux types de sonde pour mesurer des vitesses dans des métaux liquides. Nous montrons aussi par des mesures locales et globales comment un champ magnétique fort modifie la structure et la dynamique des écoulement tourbillonnaires de von Karman.