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.

This thesis aims a critical reading of two American series also aired in Brazil: Star Trek and Heroes. The survey proposes to observe dissensus from the multitude present on both TV series. The multitude (HARDT; NEGRI, 2000) is a social force capable of challenging the sovereign power and to establish new forms of social organization, their presence may present dissensus (RANCIÈRE, 2010), new elements to what is conventionally considered and sense, the sensitive system already established. This movement is associated with materialistic conception of history that suggests seeking tensions against the dominant social order (BENJAMIN, 1987). The Star Trek series debuted in 1966 and its last episode was broadcast in 1969. The series was produced by Desilu Productions and broadcast by NBC, and your transmission took place at a time when American foreign policy has to tend less to an imperialist activity than to a policing action to a supranational order service. The hypothesis is that his narrative shows the will of the multitude to prevent the exercise of the former European sovereignty and to overcome the nationalist struggles. The Heroes series was produced in partnership by Tailwind Productions, NBC, Universal Television and Universal Media Studios. Four seasons were exhibited from 2006 to 2009. The series covers the history of characters who, because of genetic mutations, discover powers that make them special. Although they appear in different parts of the world, there is some force that, in many ways, remains interconnection between the characters. The hypothesis is that the special abilities of Heroes characters may be attached to faculties of the multitude able to oppose the order of global capitalism. The overall objective of this research is, as stated initially, to look for dissensus from multitude inside the series. It is possible to see that these cultural objects do not carry a single system of presentation attached to commercial logic, but let see, within their respective contexts of production, transformative capacities against the established order. It can be said that the tensions in the series denote trouble for tradition defended by the dominator, presenting challenging ways to read the story doing justice to the dominated. / Submitted by Carolini da Rocha (carolini.rocha@unisul.br) on 2017-05-09T12:50:52Z No. of bitstreams: 2 jeanrzhoullou.pdf: 2355014 bytes, checksum: 53c7c03bc132c6a3dc6fa6c11cf22807 (MD5) Jean Raphael Zimmermann Houllou.pdf: 770947 bytes, checksum: 818c2879f4b96ee04555885d98022d3e (MD5) / Approved for entry into archive by Carolini da Rocha (carolini.rocha@unisul.br) on 2017-05-09T12:52:32Z (GMT) No. of bitstreams: 2 jeanrzhoullou.pdf: 2355014 bytes, checksum: 53c7c03bc132c6a3dc6fa6c11cf22807 (MD5) Jean Raphael Zimmermann Houllou.pdf: 770947 bytes, checksum: 818c2879f4b96ee04555885d98022d3e (MD5) / Made available in DSpace on 2017-05-09T12:52:32Z (GMT). No. of bitstreams: 2 jeanrzhoullou.pdf: 2355014 bytes, checksum: 53c7c03bc132c6a3dc6fa6c11cf22807 (MD5) Jean Raphael Zimmermann Houllou.pdf: 770947 bytes, checksum: 818c2879f4b96ee04555885d98022d3e (MD5) Previous issue date: 2016 / A presente tese pretende uma leitura crítica de dois seriados norte-americanos, também veiculados no Brasil: Star Trek e Heroes. O exame propõe observar dissensos da multidão presentes em ambos os seriados de TV. A multidão (HARDT; NEGRI, 2000) é como uma força social capaz de desafiar o poder soberano e instituir novas formas de organização social; sua presença pode apresentar dissensos (RANCIÈRE, 2010), ou seja, novos elementos para aquilo que convencionalmente é considerado e sentido, o regime do sensível já estabelecido. Esse movimento se associa a concepção de história materialista que sugere a procura de tensões contra a ordem social dominante (BENJAMIN, 1987). O seriado Star Trek estreou em 1966 e seu último episódio foi transmitido em 1969. A série foi produzida pela Desilu Productions e exibida pela NBC, e sua transmissão se deu num momento em que a política externa americana passou a tender menos para uma atividade imperialista do que para uma ação de policiamento a serviço de uma ordem supranacional. A hipótese é a de que sua narrativa apresenta a vontade da multidão em impedir o exercício da antiga soberania europeia e em superar as lutas nacionalistas. O seriado Heroes foi produzido em parceria pela Tailwind Productions, NBC,Universal Television e Universal Media Studios. Foram exibidas quatro temporadas de 2006 a 2009. A série aborda a história de personagens que, em razão de mutações genéticas, se descobrem portadores de poderes que os tornam especiais. Embora apareçam em diferentes partes do mundo, existe alguma força que, de variadas formas, mantém os personagens interconectados. A hipótese em Heroes é a de que as habilidades especiais dos personagens podem ser associadas às faculdades da multidão capazes de se opor à ordem do capitalismo global. O objetivo geral desta pesquisa consiste, como afirmado inicialmente, em averiguar dissensos da multidão dentro dos seriados. É possível observar que estes objetos da cultura não carregam um regime único de apresentação ligado à lógica mercantil, mas permitem constatar, dentro de seus respectivos contextos de produção, capacidades transformadoras contra a ordem constituída. Pode-se afirmar que as tensões observadas nos seriados denotam problemas para a tradição defendida pelo dominador apresentando formas desafiadoras à leitura da história e fazendo justiça aos dominados.

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.

abstract: Green pea galaxies are a class of rare, compact starburst galaxies that have powerful optical emission line [OIII]$\lambda$5007. They are the best low-redshift analogs of high-redshift (z$>$2) Lyman-alpha emitting galaxies (LAEs). They provide unique opportunities to study physical conditions in high-redshift LAEs in great detail. In this dissertation, a few physical properties of green peas are investigated. The first study in the dissertation presents star formation rate (SFR) surface density, thermal pressure in HII regions, and a correlation between them for 17 green peas and 19 Lyman break analogs, which are nearby analogs of high-redshift Lyman break galaxies. This correlation is consistent with that found from the star-forming galaxies at z $\sim$ 2.5. In the second study, a new large sample of 835 green peas in the redshift range z = 0.011 -- 0.411 are assembled from Data Release 13 of the Sloan Digital Sky Survey (SDSS) with the equivalent width of the line [OIII]$\lambda$5007 $>$ 300\AA\ or the equivalent width of the line H$\beta$ $>$ 100\AA. The size of this new sample is ten times that of the original 80 star-forming green pea sample. With reliable T$_e$-based gas-phase metallicity measurements for the 835 green peas, a new empirical calibration of R23 (defined as ([OIII]$\lambda$$\lambda$4959,5007 + [OII]$\lambda$$\lambda$3726,3729)/H$\beta$) for strong line emitters is then derived. The double-value degeneracy of the metallicity is broken for galaxies with large ionization parameter (which manifests as log([OIII]$\lambda$$\lambda$4959,5007/[OII]$\lambda$$\lambda$3726,3729) $\geq$ 0.6). This calibration offers a good way to estimate metallicities for extreme emission-line galaxies and high-redshift LAEs. The third study presents stellar mass measurements and the stellar mass-metallicity relation of 828 green peas from the second study. The stellar mass covers 6 orders of magnitude in the range 10$^{5}$ -- 10$^{11}$ M$_{\odot}$, with a median value of 10$^{8.8}$ M$_{\odot}$. The stellar mass-metallicity relation of green peas is flatter and displays about 0.2 - 0.5 dex offset to lower metallicities in the range of stellar mass higher than 10$^{8}$ M$_{\odot}$ compared to the local SDSS star-forming galaxies. A significant dependence of the stellar mass-metallicity relation on star formation rate is not found in this work. / Dissertation/Thesis / Doctoral Dissertation Astrophysics 2018

Ma thèse est centrée sur l'étude de l'interaction entre les étoiles massives et le milieu environnant. Je suis particulièrement intéressé par l'effet qu'ont ces étoiles sur les jeunes objets stellaires observés autour d'elles. Les étoiles massives forment des régions d'hydrogène ionisé (HII) dont l'expansion supersonique conduit à la formation d'une couche de gaz et de poussières où les conditions paraissent favoriser la formation stellaire. Mon travail consiste à étudier les propriétés des jeunes objets stellaires autour de ces régions HII et à savoir si la région HII a influencé positivement la formation de ces sources.En utilisant les données Herschel, issues des programmes HOBYS et Hi-GAL, complétées par d'autres observations, j'ai étudié deux régions HII galactiques (RCW~79 et RCW~120) afin de caractériser la formation stellaire observée à leurs frontières. Pour étudier l'impact de la photoionisation, j'ai calculé le taux de formation stellaire (SFR) pour ces deux régions. Cette grandeur suggère que RCW~79 et RCW~120 sont des régions de formation stellaire actives malgré leur relative faible densité surfacique de gaz. Une nouvelle étude de la région G345 est en cours. Cette région HII est située au-dessus du plan galactique et forme activement des étoiles. Avec les données disponibles, les propriétés de la formation stellaire seront discutées. Cette étude nous donne l'opportunité de mieux comprendre les effets de la photoionisation en dehors du plan galactique. Cette région viendra augmenter notre échantillon de régions HII, ce qui est nécessaire pour avoir une vision globale des mécanismes en jeu et pour mieux comprendre l'efficacité de la formation stellaire. / My PhD thesis deals with the study of the interaction between high mass stars and their surrounding medium. I am particularly interested in the way high-mass stars affect the young stars observed around them. Massive stars form ionized (HII) regions which, during their supersonic expansion, lead to the formation of a layer of gas and dust where the conditions seem to favor star formation. My work aims at understanding the properties of star formation around Galactic HII regions.Using \herschel\, data (HOBYS and Hi-GAL programs) complemented with ancillary data, I studied two Galactic \HII\, regions (RCW~79 and RCW~120) to characterize the star formation observed at their edges. To study the impact of the ionization pressure, I computed the Star Formation Rate (SFR), which suggests that RCW~79 and RCW~120 are active star-forming regions despite their low gas surface density.A new study about the G345 region is in progress. This HII region is located above the Galactic plane and is actively forming stars. With the data available, the star formation's properties is being derived such as the spatial distribution of clumps, their stellar content, the SFR and CFE. This new study offers another opportunity to better understand the photoionization feedback out of the Galactic plane. Moreover, this will complete the sample of detailed studies of \HII\, regions, allowing us to obtain a global view of the mechanisms at play and of the efficiency of star formation in these regions.

Context: Unmanned Aerial Vehicles are being widely being used for various scientific and non-scientific purposes. This increases the need for effective and efficient path planning of Unmanned Aerial Vehicles.Two of the most commonly used methods are the A-star algorithm and Mixed Integer Linear Programming.Objectives: Conduct a simulation experiment to determine the performance of A-star algorithm and Mixed Integer Linear Programming for path planning of Unmanned Aerial Vehicle in a simulated environment.Further, evaluate A-star algorithm and Mixed Integer LinearProgramming based computational time and computational space to find out the efficiency. Finally, perform a comparative analysis of A star algorithm and Mixed Integer Linear Programming and analyse the results.Methods: To achieve the objectives, both the methods are studied extensively, and test scenarios were generated for simulation of Objectives: Conduct a simulation experiment to determine the performance of A-star algorithm and Mixed Integer Linear Programming for path planning of Unmanned Aerial Vehicle in a simulated environment.Further, evaluate A-star algorithm and Mixed Integer LinearProgramming based computational time and computational space to find out the efficiency. Finally, perform a comparative analysis of A star algorithm and Mixed Integer Linear Programming and analyse the results.Methods: To achieve the objectives, both the methods are studied extensively, and test scenarios were generated for simulation of Methods: To achieve the objectives, both the methods are studied extensively, and test scenarios were generated for simulation of these methods. These methods are then implemented on these test scenarios and the computational times for both the scenarios were observed.A hypothesis is proposed to analyse the results. A performance evaluation of these methods is done and they are compared for a better performance in the generated environment. Results: It is observed that the efficiency of A-star algorithm andMILP algorithm when no obstacles are considered is 3.005 and 12.03functions per second and when obstacles are encountered is 1.56 and10.59 functions per seconds. The results are statistically tested using hypothesis testing resulting in the inference that there is a significant difference between the computation time of A-star algorithm andMILP. Performance evaluation is done, using these results and the efficiency of algorithms in the generated environment is obtained.Conclusions: The experimental results are analysed, and the Conclusions: The experimental results are analysed, and the efficiencies of A-star algorithm and Mixed Integer Linear Programming for a particular environment is measured. The performance analysis of the algorithm provides us with a clear view as to which algorithm is better when used in a real-time scenario. It is observed that Mixed IntegerLinear Programming is significantly better than A-star algorithm.

We present an extremely deep CO(1-0) observation of a confirmed z = 1.62 galaxy cluster. We detect two spectroscopically confirmed cluster members in CO(1-0) with signal-to-noise ratio >5. Both galaxies have log (M-star/M-circle dot) > 11 and are gas rich, with M-mol/(M-star + M-mol) similar to 0.17-0.45. One of these galaxies lies on the star formation rate (SFR)-M-star sequence, while the other lies an order of magnitude below. We compare the cluster galaxies to other SFR-selected galaxies with CO measurements and find that they have CO luminosities consistent with expectations given their infrared luminosities. We also find that they have gas fractions and star formation efficiencies (SFE) comparable to what is expected from published field galaxy scaling relations. The galaxies are compact in their stellar light distribution, at the extreme end for all high-redshift star-forming galaxies. However, their SFE is consistent with other field galaxies at comparable compactness. This is similar to two other sources selected in a blind CO survey of the HDF-N. Despite living in a highly quenched protocluster core, the molecular gas properties of these two galaxies, one of which may be in the process of quenching, appear entirely consistent with field scaling relations between the molecular gas content, stellar mass, star formation rate, and redshift. We speculate that these cluster galaxies cannot have any further substantive gas accretion if they are to become members of the dominant passive population in z < 1 clusters.

Esta dissertação apresenta uma breve revisão introdutória de alguns aspectos importantes de astrofísica nuclear e da fenomenologia do plasma de quarks e glúons a baixas temperaturas. Acredita-se que tal estado da matéria existe no núcleo de estrelas de nêutron e possivelmente de outros objetos compactos em astrofísica. Uma equação de estado para tal sistema é derivada incluindo as influências dos condensados de glúon e do campo magnético que também é uma característica importante das estrelas de nêutron. Finalmente, essa equação de estado é aplicada para o estudo de estrutura estelar de estrelas compactas e alguns resultados importantes são discutidos. / This dissertation presents a brief introductory overview of some key aspects of nuclear astrophysics and of the phenomenology of the quark gluon plasma at cold temperatures which is believed to exist inside the core of neutron stars and possible other compact astrophysical objects. An equation of state for this state of matter is derived incluing the influence of gluon condensates and the magnetic field which is also an important characteristic of neutron stars. And finally this equation of state is applied to the study of compact stellar structure and some important results are discussed.