abstract: Among the various end-use sectors, the commercial sector is expected to have the second-largest increase in total primary energy consump¬tion from 2009 to 2035 (5.8 quadrillion Btu) with a growth rate of 1.1% per year, it is the fastest growing end-use sectors. In order to make major gains in reducing U.S. building energy use commercial sector buildings must be improved. Energy benchmarking of buildings gives the facility manager or the building owner a quick evaluation of energy use and the potential for energy savings. It is the process of comparing the energy performance of a building to standards and codes, to a set target performance or to a range of energy performance values of similar buildings in order to help assess opportunities for improvement. Commissioning of buildings is the process of ensuring that systems are designed, installed, functionally tested and capable of being operated and maintained according to the owner's operational needs. It is the first stage in the building upgrade process after it has been assessed using benchmarking tools. The staged approach accounts for the interactions among all the energy flows in a building and produces a systematic method for planning upgrades that increase energy savings. This research compares and analyzes selected benchmarking and retrocommissioning tools to validate their accuracy such that they could be used in the initial audit process of a building. The benchmarking study analyzes the Energy Use Intensities (EUIs) and Ratings assigned by Portfolio Manager and Oak Ridge National Laboratory (ORNL) Spreadsheets. The 90.1 Prototype models and Commercial Reference Building model for Large Office building type were used for this comparative analysis. A case-study building from the DOE - funded Energize Phoenix program was also benchmarked for its EUI and rating. The retrocommissioning study was conducted by modeling these prototype models and the case-study building in the Facility Energy Decision System (FEDS) tool to simulate their energy consumption and analyze the retrofits suggested by the tool. The results of the benchmarking study proved that a benchmarking tool could be used as a first step in the audit process, encouraging the building owner to conduct an energy audit and realize the energy savings potential. The retrocommissioning study established the validity of FEDS as an accurate tool to simulate a building for its energy performance using basic inputs and to accurately predict the energy savings achieved by the retrofits recommended on the basis of maximum LCC savings. / Dissertation/Thesis / M.S. Architecture 2011

abstract: Most stars form in groups, and these clusters are themselves nestled within larger associations and stellar complexes. It is not yet clear, however, whether stars cluster on preferred size scales within galaxies, or if stellar groupings have a continuous size distribution. I have developed two methods to select stellar groupings across a wide range of size-scales in order to assess trends in the size distribution and other basic properties of stellar groupings. The first method uses visual inspection of color-magnitude and color-color diagrams of clustered stars to assess whether the compact sources within the potential association are coeval, and thus likely to be born from the same parentmolecular cloud. This method was developed using the stellar associations in the M51/NGC 5195 interacting galaxy system. This process is highly effective at selecting single-aged stellar associations, but in order to assess properties of stellar clustering in a larger sample of nearby galaxies, an automated method for selecting stellar groupings is needed. I have developed an automated stellar grouping selection method that is sensitive to stellar clustering on all size scales. Using the Source Extractor software package on Gaussian-blurred images of NGC 4214, and the annular surface brightness to determine the characteristic size of each cluster/association, I eliminate much of the size and density biases intrinsic to other methods. This automated method was tested in the nearby dwarf irregular galaxy NGC 4214, and can detect stellar groupings with sizes ranging from compact clusters to stellar complexes. In future work, the automatic selection method developed in this dissertation will be used to identify stellar groupings in a set of nearby galaxies to determine if the size scales for stellar clustering are uniform in the nearby universe or if it is dependent on local galactic environment. Once the stellar clusters and associations have been identified and age-dated, this information can be used to deduce disruption times from the age distribution as a function of the position of the stellar grouping within the galaxy, the size of the cluster or association, and the morphological type of the galaxy. The implications of these results for galaxy formation and evolution are discussed. / Dissertation/Thesis / Ph.D. Astrophysics 2011

Les jeunes amas d'étoiles sont sous-structurés et évoluent dynamiquement pour former des amas sphériques à l'équilibre. Je présente une nouvelle méthode pour générer des conditions initiales réalistes pour simuler ce processus: la fragmentation de Hubble-Lemaitre. Je laisse le système développer spontanément des surdensités au cours d'une expansion du système. Le modèle résultant se compare bien aux simulations hydrodynamiques de formation stellaire et aux observations des jeunes amas. Le modèle fragmenté s'effondre de manière plus douce qu'un modèle uniforme. L'injection d'une population d'étoile binaire avant l'effondrement a montré qu'un système sous-structuré détruisait bien plus de binaires qu'un système à l'équilibre. Des binaires particulièrement larges ou serrées, jusqu’à 0.01 AU, ont également été détectées dans ces modèles. Cette méthode est très prometteuse, un exemple d'application est la génération d'observations synthétiques de régions de formation stellaire. / Young star clusters are substructured and undergo a dynamical evolution erasing this substructure to form relaxed spherical clusters. I present a new method to generate realistic initial conditions to perform N-body simulations of this process: the Hubble-Lemaitre fragmentation. By expanding an initially uniform sphere, I allow spontaneous overdensities to grow, creating a realistic model for young clumpy stellar systems. This method is validated by analysing the distribution and content of the clumps and comparing them to hydrodynamical simulations of star formation as well as observations of star forming regions. These systems undergo a softer collapse than uniform ones. I injected binary stars in the fragmented models and found they were heavily processed when substructure was present. I also found extreme short and tight binaries, down to 0.01 AU, to formin the models. The method has a lot of potential, such as the generation of mock observations of star-forming regions.

This diploma thesis focuses on matters of stereotyping of documentary portraits depicting pop music icons. The theoretical part of the thesis deals with issues such as stereotyping as part of media representation of reality, and the definition of term "celebrity" and its specifics in the context of music industry. The term "documentary portrait" is also grasped theoretically. The practical part of the thesis introduces the documentary films which were examined. The methodology of the research and its design are described as well. The final part of the thesis consists of a research report, which includes results acquired by a qualitative survey on the basis of a grounded theory method.

White dwarf stars are the most common final stage of stellar evolution, corresponding to 99% of all stars in the Galaxy. White dwarf models can be used to obtain the age of stellar populations, to build an initial to final mass relation to understand the connection between the properties of white dwarfs and their progenitors, determine the upper mass limit that separates white dwarfs progenitors from Type II supernovae, enhance the comprehension of the physical properties of high density matter and derive ages and masses for observed white dwarfs from the cooling tracks. The literature is populated with low mass and intermediate mass white dwarf models, however the massive white dwarfs are often forgotten and the evolutionary sequences are incomplete. In this dissertation, we compute full evolutionary sequences for massive white dwarfs, exploring the evolution of hydrogen-rich and hydrogen-deficient white dwarfs stars with masses between 1.012 and 1.307 M , and initial metallicity of Z = 0.02. These sequences are the result of main sequence stars with masses between 8.8 and 11.8 M . The simulations were performed with the Modules for Experiments in Stellar Astrophysics - MESA code, starting at the zero-age main sequence, through thermally pulsing and mass-loss phases, ending as the white dwarfs at the cooling sequence. Our simulations are full evolutionary, in which we consider the entire evolutionary history of the progenitors. We present reliable nuclear chemical profiles for the whole mass range considered, covering the different expected central compositions, i.e. C/O, O/Ne and Ne/O/Mg, and their dependence with the stellar mass. In addition, we present detailed chemical profiles of hybrid C/O-O/Ne core white dwarfs, found in the mass range between 1.024 and 1.150 M . We present the initial-to-final mass relation, mass-radius relation, and cooling times with improved crystallization limits, considering the effects of atmosphere and core composition.

Remarkable progress has been made over the last few decades in furthering our understanding of the growth of cosmic structure. Nonetheless, there remains a great deal of uncertainty regarding the precise details of the complex baryonic physics that regulate galaxy formation. Any theory of star formation in galaxies must encompass the radiative cooling of gas into dark matter haloes, the formation of a turbulent, multiphase interstellar medium (ISM), the efficiency with which molecular gas is able to collapse into cores and ultimately stars, and the subsequent interaction of those stars with the gas through ionizing radiation, winds and supernova (SN) explosions. Given the highly non-linear nature of the problem, numerical simulations provide an invaluable tool with which to study galaxy formation. Yet, even with contemporary computational resources, the inherently large dynamical range of spatial scales that must be tackled makes the development of such models extremely challenging, inevitably leading to the adoption of `subgrid' approximations at some scale. In this thesis, I explore new methods of incorporating the physics of star formation and stellar feedback into high resolution hydrodynamic simulations of galaxies. I first describe a new implementation of star formation and SN feedback that I have developed for the state-of-the-art moving mesh code Arepo. I carry out a detailed study into various classes of subgrid SN feedback schemes commonly adopted in the literature, including injections of thermal and/or kinetic energy, two parametrizations of delayed cooling feedback and a 'mechanical' feedback scheme that injects the appropriate amount of momentum depending on the relevant scale of the SN remnant (SNR) resolved. All schemes make use of individually time-resolved SN events. Adopting isolated disk galaxy setups at different resolutions, with the highest resolution runs reasonably resolving the Sedov-Taylor phase of the SNR, I demonstrate that the mechanical scheme is the only physically well-posed method of those examined, is efficient at suppressing star formation, agrees well with the Kennicutt-Schmidt relation and leads to converged star formation rates and galaxy morphologies with increasing resolution without fine tuning any parameters. However, I find that it is difficult to produce outflows with high enough mass loading factors at all but the highest resolution. I discuss the various possible solutions to this effect, including improved modelling of star formation. Moving on to a more self-consistent setup, I carry out a suite of cosmological zoom-in simulations of low mass haloes at very high resolution, performed to z = 4, to investigate the ability of SN feedback models to produce realistic galaxies. The haloes are selected in a variety of environments, ranging from voids to crowded locations. In the majority of cases, SN feedback alone has little impact at early times even in low mass haloes ($\sim10^{10}\,\mathrm{M_\odot}$ at z = 0). This appears to be due largely to the build up of very dense gas prior to SN events, suggesting that other mechanisms (such as other stellar feedback processes) are required to regulate ISM properties before SNe occur. The effectiveness of the feedback also appears to be strongly dependent on the merger history of the halo. Finally, I describe a new scheme to drive turbulence in isolated galaxy setups. The turbulent structure of the ISM very likely regulates star formation efficiencies on small scales, as well as affecting the clustering of SNe. The large range of potential drivers of ISM turbulence are not fully understood and are, in any case, unlikely to arise ab initio in a whole galaxy simulation. I therefore neglect these details and adopt a highly idealised approach, artificially driving turbulence to produce an ISM structure of my choice. This enables me to study the effects of a given level of ISM turbulence on global galaxy properties, such as the fragmentation scale of the disk and the impact on SN feedback efficiencies. I demonstrate this technique in the context of simulations of isolated dwarfs, finding that moderate levels of turbulent driving in combination with SN feedback can produce a steady-state of star formation rates and global galaxy properties, rather than the extremely violent SN feedback that is produced by a rapidly fragmenting disk.

A cultura da convergência abarca a questão tecnológica do fluxo de conteúdos, ocorrendo através de múltiplos suportes midiáticos e as questões de mudança de comportamento do público, que se apropria das redes digitais para buscar de diferentes experiências de entretenimento e de informação. Os sujeitos buscam um produto midiático que não se finde na sua própria exibição, mas sim proponha conteúdos que vão além de um único dispositivo de distribuição e necessitem do engajamento do público para que aconteçam efetivamente. Os fãs são personagens centrais da mudança na forma de operar da mídia de massa por serem pioneiros na adaptação às novas tecnologias de comunicação e informação e nos processos de produção e consumo participativos. A partir disso, esta pesquisa busca um olhar sobre as interações que fazem parte do comportamento dos fãs, tanto nas relações entre eles quanto com a indústria midiática. Para tanto, estudam-se os fãs de Star Wars, mais especificamente, os membros do Conselho Jedi do Rio Grande do Sul (CJRS), a fim de que através de um objeto empírico, consolidado e permanente se possa investigar o comportamento deste grupo no contexto de cultura da convergência, onde as interações entre eles e com o mercado de mídia são transformadas. / The convergence culture includes the technological issue of the content flow going through multiple media and the issues of changes in public behavior which appropriates itself of the digital networks seeking for different experiences of entertainment and information. The individuals look for a media product that doesn‟t finish itself in its own exhibition, but propose content that go beyond a single distribution device and require the engagement of the audience to actually happen. The fans are central characters in the change of mass media operating way because they are pioneers in adapting the new technologies of communication and information and in participatory processes of production and consumption. From this, this research seeks a look at the interactions that are part of the behavior of fans, both in relations between them and with the media industry. To this end, the Star Wars fans are studied, more specifically, the members of the Jedi Council of Rio Grande do Sul (CJRS), so that through a consolidated and permanent empirical object, it became possible to investigate the behavior of this group in the convergence culture context where the interactions between them and the media market are changed.

A cultura da convergência abarca a questão tecnológica do fluxo de conteúdos, ocorrendo através de múltiplos suportes midiáticos e as questões de mudança de comportamento do público, que se apropria das redes digitais para buscar de diferentes experiências de entretenimento e de informação. Os sujeitos buscam um produto midiático que não se finde na sua própria exibição, mas sim proponha conteúdos que vão além de um único dispositivo de distribuição e necessitem do engajamento do público para que aconteçam efetivamente. Os fãs são personagens centrais da mudança na forma de operar da mídia de massa por serem pioneiros na adaptação às novas tecnologias de comunicação e informação e nos processos de produção e consumo participativos. A partir disso, esta pesquisa busca um olhar sobre as interações que fazem parte do comportamento dos fãs, tanto nas relações entre eles quanto com a indústria midiática. Para tanto, estudam-se os fãs de Star Wars, mais especificamente, os membros do Conselho Jedi do Rio Grande do Sul (CJRS), a fim de que através de um objeto empírico, consolidado e permanente se possa investigar o comportamento deste grupo no contexto de cultura da convergência, onde as interações entre eles e com o mercado de mídia são transformadas. / The convergence culture includes the technological issue of the content flow going through multiple media and the issues of changes in public behavior which appropriates itself of the digital networks seeking for different experiences of entertainment and information. The individuals look for a media product that doesn‟t finish itself in its own exhibition, but propose content that go beyond a single distribution device and require the engagement of the audience to actually happen. The fans are central characters in the change of mass media operating way because they are pioneers in adapting the new technologies of communication and information and in participatory processes of production and consumption. From this, this research seeks a look at the interactions that are part of the behavior of fans, both in relations between them and with the media industry. To this end, the Star Wars fans are studied, more specifically, the members of the Jedi Council of Rio Grande do Sul (CJRS), so that through a consolidated and permanent empirical object, it became possible to investigate the behavior of this group in the convergence culture context where the interactions between them and the media market are changed.

Master of Science / Department of Architectural Engineering and Construction Science / Julia A. Keen / The intent of this report is to recommend a process for legislation that can be used to identify commercial buildings that have the greatest potential to reduce energy consumption. A point-based evaluation is completed of current energy processes for existing commercial buildings. The recommended energy evaluation system is applied to an existing building, which allows for a detailed review of how the evaluation is completed for a building. The results are presented to display the value of assessing building energy performance. Additionally, the results reinforce the potential to transform the industry and energy use by buildings.

En 1972, Skumanich découvre une relation empirique unique entre la période de rotation de surface des étoiles G et leur âge sur la séquence principale. Cette découverte ouvrit alors une nouvelle voie pour la datation stellaire : la gyrochronologie. Dès lors, bon nombre d'auteurs, entre la fin des années 80 et 90, se sont intéressés à l'évolution de la vitesse de rotation de surface des étoiles de faible masse ($M_*$ = 0.4 $M_{odot}$- 1.1 $M_{odot}$). Les premiers modèles phénoménologies sur le sujet été nés.L'évolution de la vitesse de rotation de ces étoiles commence à être raisonnablement bien reproduite par la classe de modèle paramétrique que je présente dans cette thèse. Par manque de descriptions théoriques satisfaisantes, seuls les effets globaux des mécanismes physiques impliqués sont ici décris. Le principal enjeu est d'étudier le cadre et la façon dont le moment cinétique stellaire est impacté par ces processus tout en contraignant leurs principales caractéristiques.Au cours de ma thèse, j'ai modélisé les trajets rotationnels des enveloppes externes et médianes des distributions de période de rotation de 18 amas stellaire entre 1 Myr et 1 Gyr. Ceci m'a permis d'analyser la dépendance temporelle des mécanismes physiques impliqués dans l'évolution du moment cinétique des étoiles de type solaire. Les résultats que j'ai obtenus montrent que l'évolution de la rotation différentielle interne impact fortement la convergence rotationnelle (relation empirique de Skumanich), l'évolution de l'abondance de surface en lithium, et les intensités du champ magnétique généré par effet dynamo. En plus de reproduire ces enveloppes externes, le modèle que j'ai développé fournit des contraintes sur les mécanismes de redistribution interne du moment cinétique et sur les durées de vie des disques circumstellaires, supposés responsables de la régulation rotationnelle observée durant les quelques premiers millions d'années de la pré-séquence principale. L'extension du modèle aux étoiles moins massives (0.5 et 0.8 $M_{odot}$) que j'ai réalisé, a également fournis la dépendance en masse de ces différents processus physiques.Cette étape à notamment ajoutée de fortes contraintes sur les temps caractéristiques associés au transport de moment cinétique entre le coeur et l'enveloppe, sur l'efficacité du freinage magnétique vraisemblablement reliée à un changement de topologie des étoiles de type solaire vers celles de 0.5 $M_{odot}$, et sur l'histoire rotationnelle, interne comme de surface, des étoiles entre 1 Myr à 1 Gyr. / In 1972, Skumanich discovers a unique empirical relationship between the rotation period of the surface of G star and their age on the main sequence. This discovery then opened a new path for stellar dating: the gyrochronology. Therefore, many authors in the late 80's and the begenning 90's, were interested in the evolution of the surface angular velocity of low-mass stars ($M_*$ = 0.4 $M_{odot}$- 1.1 $M_{odot}$). The first phenomenological models on the subject were born.The angular velocity evolution of these stars begins to be reasonably well reproduced by the class of parametrical model that I present in this thesis. Because of the lack of adequate theoretical descriptions, only the overall effects of the physical mechanisms involved are described here. The main issue is to study the framework and how the stellar angular momentum is affected by these processes and to constrain their main characteristics.Over the course of my thesis, I modelled the rotational tracks of external and median envelopes and median of rotation period distributions of 18 stellar clusters between 1 Myr and 1 Gyr. This allowed me to analyse the time dependence of the physical mechanisms involved in the angular momentum evolution of solar-type stars. The results I obtained show that the evolution of the internal differential rotation significantly impact the rotational convergence (empirical Skumanich's relationship), the evolution of the surface lithium abundance, and the intensity of the magnetic field generated by dynamo effect. In addition to the reproduction of these external envelopes, the model I developed provides constraints on the mechanisms of internal redistribution of angular momentum and the lifetimes of circumstellar disks, that are held responsible for the rotational regulation observed during the first few million years of pre-main sequence. The extension of the model to less massive stars (0.5 et 0.8 $M_{odot}$) that I performed also provided the mass dependence of these physical processes. Most specifically, this step added strong constraints on the characteristic time associated to the transport of angular momentum between the core and the envelope, on the efficiency of magnetic braking likely related to a change of topology from solar-type stars to those of 0.5 $M_{odot}$, and on the internal and external rotational history of stars from 1 Myr to 1 Gyr.