Made available in DSpace on 2016-06-02T20:23:14Z (GMT). No. of bitstreams: 1 5087.pdf: 3337839 bytes, checksum: dd1a3d8080f9c50c9ec2f2dbd7f23682 (MD5) Previous issue date: 2012-11-30 / Financiadora de Estudos e Projetos / The major media conglomerates consolidated from the 1980s invest heavily on franchises captained by blockbusters movies and a wide range of products derived from them, in search of larger profits in the worldwide entertainment market. This study aims to analyze the marketing characteristics of franchises produced by major media conglomerates. In intend to do so, notes and appointments are made on the Star Wars film franchise, referred to as a kind of genesis for the franchise business model that the entertainment industry practices today. Star Wars created a paradigm in the production process of the Hollywood studios, combining filmic creativity with product marketing practices for disclosure and especially the development of strategic marketing licensing and merchandising of products that carry its brand. Through the analysis of the narrative structure of the Star Wars movies, creative tools used in the development of the story and its characters are identified showing possible paths for creating extensions and sequences that allow the expansion of several derived products across multiple platforms, building the media franchise. / Os grandes conglomerados de mídia, consolidados a partir da década de 1980, investem pesadamente em franquias capitaneadas por filmes blockbusters e uma vasta gama de produtos deles derivados, na busca de lucros cada vez maiores no mercado do entretenimento mundial. Este trabalho tem por objetivo analisar as características mercadológicas das franquias produzidas pelos grandes conglomerados de mídia, tendo como objeto de estudo e apontamentos a franquia cinematográfica Star Wars, referenciada como uma espécie de gênese para o modelo de negócio de franquias que a indústria do entretenimento pratica hoje. Star Wars criou um paradigma no processo produtivo dos estúdios de Hollywood, unindo a criatividade do produto fílmico com as práticas de marketing para sua divulgação e, principalmente, o desenvolvimento de estratégicas mercadológicas de licenciamento e de merchandising dos produtos que levam sua marca. Por meio da análise da estrutura narrativa dos filmes de Star Wars, são identificadas ferramentas que, utilizadas no desenvolvimento da história e de seus personagens, possibilitam caminhos para a criação de extensões e sequências na expansão dos vários produtos derivados, em diversas plataformas, na construção da franquia de mídia.

O objetivo desta dissertação é analisar a cobertura jornalística ao cinema brasileiro durante os anos cinqüenta em duas revistas de fãs: A Cena Muda (1921-1955) e Cinelândia (1952-1967), avaliando a estrutura da crítica cinematográfica e seu papel como geradora do star system brasileiro. A análise do material de nosso estudo congrega os anos de 1952 a 1955, único período em que as duas publicações coexistiram. Através da análise comparativa com a cobertura ao cinema de Hollywood, traçamos os paralelos da configuração do estrelismo brasileiro, com especial atenção às estratégias de legitimação do sistema para aumentar o interesse dos leitores e às peculiaridades da crítica em lidar com o star system. / This dissertation has by finality the study of the journalistic coverage to the brazilian cinema during the fifties in two fan magazines: A Cena Muda (1921-1955) and Cinelândia (1952-1967) to assess the structure of the critic cinematograph and their role as producer of brazilian star system. The material analysis of our study assembles the years of 1952 to 1955, only period in which both publications coexisted. Through the comparative analysis with the coverage of the Hollywood cinema, we draw the parallel with the configurations of brazilian star system, with special interest to the system legitimacy strategies to increase the readers interest and to the peculiarities of the critic to handle with the star system.

Com o crescimento do volume de dados manipulado por aplicações de data warehousing, soluções centralizadas tornam-se muito custosas e enfrentam dificuldades para tratar a escalabilidade do volume de dados. Nesse sentido, existe a necessidade tanto de se armazenar grandes volumes de dados quanto de se realizar consultas analíticas (ou seja, consultas OLAP) sobre esses dados volumosos de forma eficiente. Isso pode ser facilitado por cenários caracterizados pelo uso de bancos de dados NoSQL gerenciados em ambientes paralelos e distribuídos. Dentre os desafios relacionados a esses cenários, destaca-se a necessidade de se promover uma análise de desempenho de aplicações de data warehousing que armazenam os dados do data warehouse (DW) em bancos de dados NoSQL orientados a colunas. A análise experimental e padronizada de diferentes sistemas é realizada por meio de ferramentas denominadas benchmarks. Entretanto, benchmarks para DW foram desenvolvidos majoritariamente para bancos de dados relacionais e ambientes centralizados. Nesta pesquisa de mestrado são investigadas formas de se estender o Star Schema Benchmark (SSB), um benchmark de DW centralizado, para o banco de dados NoSQL distribuído e orientado a colunas HBase. São realizadas propostas e análises principalmente baseadas em testes de desempenho experimentais considerando cada uma das quatro etapas de um benchmark, ou seja, esquema e carga de trabalho, geração de dados, parâmetros e métricas, e validação. Os principais resultados obtidos pelo desenvolvimento do trabalho são: (i) proposta do esquema FactDate, o qual otimiza consultas que acessam poucas dimensões do DW; (ii) investigação da aplicabilidade de diferentes esquemas a cenários empresariais distintos; (iii) proposta de duas consultas adicionais à carga de trabalho do SSB; (iv) análise da distribuição dos dados gerados pelo SSB, verificando se os dados agregados pelas consultas OLAP estão balanceados entre os nós de um cluster; (v) investigação da influência de três importantes parâmetros do framework Hadoop MapReduce no processamento de consultas OLAP; (vi) avaliação da relação entre o desempenho de consultas OLAP e a quantidade de nós que compõem um cluster; e (vii) proposta do uso de visões materializadas hierárquicas, por meio do framework Spark, para otimizar o desempenho no processamento de consultas OLAP consecutivas que requerem a análise de dados em níveis progressivamente mais ou menos detalhados. Os resultados obtidos representam descobertas importantes que visam possibilitar a proposta futura de um benchmark para DWs armazenados em bancos de dados NoSQL dentro de ambientes paralelos e distribuídos. / Due to the explosive increase in data volume, centralized data warehousing applications become very costly and are facing several problems to deal with data scalability. This is related to the fact that these applications need to store huge volumes of data and to perform analytical queries (i.e., OLAP queries) against these voluminous data efficiently. One solution is to employ scenarios characterized by the use of NoSQL databases managed in parallel and distributed environments. Among the challenges related to these scenarios, there is a need to investigate the performance of data warehousing applications that store the data warehouse (DW) in column-oriented NoSQL databases. In this context, benchmarks are widely used to perform standard and experimental analysis of distinct systems. However, most of the benchmarks for DW focus on relational database systems and centralized environments. In this masters research, we investigate how to extend the Star Schema Benchmark (SSB), which was proposed for centralized DWs, to the distributed and column-oriented NoSQL database HBase. We introduce proposals and analysis mainly based on experimental performance tests considering each one of the four steps of a benchmark, i.e. schema and workload, data generation, parameters and metrics, and validation. The main results described in this masters research are described as follows: (i) proposal of the FactDate schema, which optimizes queries that access few dimensions of the DW; (ii) investigation of the applicability of different schemas for different business scenarios; (iii) proposal of two additional queries to the SSB workload; (iv) analysis of the data distribution generated by the SSB, verifying if the data aggregated by OLAP queries are balanced between the nodes of a cluster; (v) investigation of the influence caused by three important parameters of the Hadoop MapReduce framework in the OLAP query processing; (vi) evaluation of the relationship between the OLAP query performance and the number of nodes of a cluster; and (vii) employment of hierarchical materialized views using the Spark framework to optimize the processing performance of consecutive OLAP queries that require progressively more or less aggregated data. These results represent important findings that enable the future proposal of a benchmark for DWs stored in NoSQL databases and managed in parallel and distributed environments.

Nesta dissertação, estuda-se estrelas compactas constituídas por uma forma estável do plasma ultra-relativístico de {\\it quarks} e glúons, a {\\it strange quark matter} ou matéria estranha, com pequena fração de elétrons para manter a neutralidade de carga. São abordadas, aqui, soluções matemáticas razoáveis que descrevem com simplicidade e agilidade certas propriedade dessas estrelas, a começar pela importantíssima relação massa-raio. Um perfil gaussiano para a densidade de energia foi escolhido como ponto de partida para contruir uma solução matemática para o problema e são apresentadas as motivações para tal escolha. Prova-se que o perfil escolhido não soluciona as Equações de Einstein exatamente e uma solução aproximada é fornecida. A seguir, as conhecidas soluções Tolman IV e Buchdahl I foram utilizadas para modelar uma estrela estranha com base no estudo de Alcock, Farhi e Olinto. Discute-se, ainda, como foi redescoberta a solução exata de Finch e Skea e discute-se, também, a solução exata para uma estrela de {\\it quarks} de Komathiraj e Maharaj, construída para um problema ligeiramente diferente, que incluía a existência de um campo elétrico. Conclui-se o trabalho comparando os resultados numéricos de Alcock, Farhi e Olinto com a solução aproximada aqui desenvolvida, apresentando o intervalo de validade desta solução. Além disso, são feitas comparações entre as diferentes soluções exatas e as características que cada uma delas exibe, e discute-se qual delas deve-se utilizar, tendo em mente que característica da estrela estranha se quer estudar. Os caminhos existentes para solucionar as Equações de Einstein, quando se quer modelar um objeto compacto, são discutidos e apontam-se quais os problemas que alguém encontrará ao seguir cada caminho. Por fim, relaciona-se a construção da relação massa-raio com a diferenciação dos tipos de objetos compactos que podem, em princípio, existir. / In this dissertation we study compact stars constituted by a stable form of ultra-relativistic quark-gluon plasma, the strange matter, with a small fraction of electrons to keep the neutrality of charge. We address here reasonable mathematical solutions that describe with simplicity and agility some properties of these stars, beginning by the important mass-radius relationship. A gaussian energy density profile was chosen as the starting point for the construction of a mathematical solution for this problem and the motivations for this choice was presented. We prove that this profile is not an exact solution for the Einstein Field Equations and an approximated solution is presented. Following, the previous known solutions of Tolman IV and Buchdahl I were used to model a strange star, based on the work of Alcock, Farhi and Olinto. We discuss the rediscovery of the exact solution of Finch and Skea and also the exact solution for a quark star by Komathiraj and Maharaj, constructed to a problem slightly different, that includes the existence of an electric field. We conclude this work comparing the numerical results of Alcock, Farhi and Olinto with the approximated solution here developed, presenting the range of validity of this solution. Furthermore, comparisons were made between the different exact solutions and the features displayed by each one and we discuss which solution must be used when one have in mind which features of the strange star one wants to study. The existent ways for solving the Einstein Equations when we want to model a compact star are discussed and we point out the problems that one will find in following each way. At last, we make a relation between the mass-radius relationship and the differentiation of the many types of compact objects that could, in principle, exist.

A star edge coloring is any edge coloring which is both proper and contains no cycles or path of length four which are bicolored, and the star chromatic index of a graph is the smallest number of colors for which that graph can be star edge colored. Star edge coloring is a relatively new field in graph theory, and very little is known regarding upper bounds of the star chromatic index of most graph types, one of these families being multipartite graphs. We investigate a method for obtaining upper bounds on the star chromatic index of complete multipartite graphs. The basic idea is to decompose such graphs into smaller complete bipartite graphs and applying known upper bounds for such graphs.This method has also been implemented and we present a hypothesis based on simulations.

We use Integral Field Unit (IFU) data for a subset of galaxies in the MaNGA (Mapping Nearby Galaxies at Apache Point Observatory) sample to investigate the environmental dependence of H-alpha properties for nearby star-forming galaxies. We characterize the non-AGN H-alpha emission for galaxies living in different host environments with radial gradient measurements, half-light radii, as well as measures of concentration and asymmetry. We find that global specific star formation rates (sSFR) are lower in nearby star-forming galaxies in groups and clusters compared to those in the field, and the lowest in high density environments such as group or cluster centres. From the resolved data we find that the overall reduction in H-alpha emission in star-forming galaxies in denser environments occurs across the face of these galaxies, suggesting starvation as a primary quenching mechanism. We further find that H-alpha disks are truncated in group galaxies that live nearer the center of the halo compared to those in the outer halo or field, which may be due to ram pressure stripping in these dense environments. / Thesis / Master of Science (MSc) / In order to understand the evolution of galaxies over time, it is necessary to determine the relative importance of external and internal factors that affect galaxy star formation. We know that galaxies in dense environments have less star formation (are quenched) compared to galaxies in the field. However, the mechanisms that dominate this quenching are less well constrained. We use a sample of galaxies in the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey to investigate the dependence of star formation on other galaxy properties as well as properties of the host environment. We find that galaxies have reduced H-alpha emission, a signature of star formation, across the entire face of the galaxy in groups and clusters compared to galaxies in the field. We further find that galaxies nearer the centre of the group or cluster halo have truncated H-alpha disks compared to galaxies in the outer part of the halo or in the field.

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No description available.

The thesis work described in this report is about simulation of the cooling of an electrical machine rotor. Limitations and simplifications were made on the CAD model of the rotor with the purpose of reducing the simulation time, for it to then be used for CFD-simulations using STAR-CCM+. This was done to see the temperature, as well as its distribution, in the model. By changing various parameters, one at the time whilst the rest were kept at their assigned standard values, the changes could be analysed and thereafter compared. The tests include smaller geometry changes, parameters of the coolant and its flow, parameters for the airgap and the materials in the laminates and the material around the magnets, as well as changes in loss values. The simulations for geometry changes involving the magnets and their surrounding material resulted in minor temperature increases. An inner rotor radius increase gave a relatively large temperature decrease (although this change would be more difficult to make in practice). Most of the mean values of the temperature changes in the regions of the model were within 10% from the standard simulation used. Increased thermal contact resistance between the Bakelite and the laminates, and increased losses had the worst impact on the cooling. Meanwhile the changes in coolant parameters (as well as the its inlet temperature and mass flow) and reduced losses had the best impact on the cooling. Generally, the temperature distributions looked similar for the different simulations. There were more differences in the distributions for the simulations with changed material properties or thermal contact resistance. / Examensarbetet som beskrivs i denna rapport handlar om simulering av kylningen av en elmaskinsrotor. Avgränsningar och vissa förenklingar gjordes på en CAD modell av rotorn för att reducera simuleringstiden. Sedan användes CFD-simuleringsprogrammet STAR-CCM+ för att simulera temperaturfördelningen i modellen. Genom att ändra olika parametrar, en åt gången medan resten hölls vid sina bestämda standardvärden, kunde förändringarna undersökas och sedan jämföras. Det som testades inkluderar bland annat mindre geometriförändringar, parametrar för kyloljan och dess flöde, parametrar för luftgapet och materialen i laminaten och runt permanentmagneterna, samt förlustförändringar. Geometriförändringarna som gjordes för magneterna och det omgivande materialet gav små temperaturökningar. En ökad inre radie på rotorn gav relativt stor temperaturminskning (men denna ändring vore svårare att genomföra på rotorn i praktiken). Majoriteten av medelvärdena av modellregionernas temperaturförändringar var inom 10% från standardsimuleringen som användes. Ökat termiskt kontaktmotstånd mellan Bakeliten och laminaten samt ökade förluster hade sämst påverkan för kylningen, medan förändring i kylvätskans egenskaperna (samt inflödestemperaturen och massflödet) samt minskade förluster hade bäst inverkan. Generellt så såg temperaturfördelningarna lika ut för de olika simuleringarna. Det var främst när materialegenskaperna eller det termiska kontaktmotståndet ändrades som fördelningen såg annorlunda ut.

<p>The formation of star clusters occurs in a complex environment and involve a large number of physical processes. One of the most important processes to consider is radiative feedback. The radiation released by forming stars heats the surrounding gas and suppresses the fragmentation of low mass objects. Ionizing radiation can also drive large scale outflows and disperse the surrounding gas. Owing to all this complexity, the use of numerical simulations to study cluster formation in molecular clouds has become commonplace. In order to study the effects of radiative feedback on cluster formation over larger spatial scales than previous studies, we present hydrodynamical simulations using the AMR code FLASH which make use of cluster particles. Unlike previous studies, these particles represent an entire star cluster rather than individual stars. We present a subgrid model for representing the radiative output of a star cluster which involves randomly sampling an IMF over time to populate the cluster. We show that our model is capable of reproducing the properties of observed clusters. The model was then incorporated into FLASH to examine the effects of radiative feedback on cluster formation in full hydrodynamical simulations. We find that the inclusion of radiative transfer can drive large scale outflows and decreases the overall star formation efficiency by a factor of 2. The inclusion of radiative feedback also increases the degree of subclustering. The use of cluster particles in hydrodynamical simulations represents a promising method for future studies of cluster formation and the large scale effects of radiative feedback.</p> / Master of Science (MSc)