Voilà plus d'un siècle que Victor Hess a montré l'origine cosmique de ce mystérieux rayonnement ionisant, et pourtant ce dernier n'a pas fini de livrer tous ces secrets. En deçà d'une énergie de l'ordre du PeV, les vestiges de supernovae sont les candidats les plus sérieux pour rendre compte de l'accélération de ces particules cosmiques. Si toutefois cette hypothèse demeure toujours d'actualité, alors qu'auparavant on le considérait comme un événement isolé dans la Galaxie, on constate plutôt aujourd'hui que ces explosions d'étoiles massives surviennent majoritairement au sein de grandes structures galactiques nommées superbulles. Ces objets sont formés par la combinaison des forts vents stellaires issus des étoiles massives ainsi que de plusieurs supernovae, tout ceci regroupé dans un espace de quelques dizaines ou centaines de parsecs.On peut dès lors se poser la question suivante : est-il possible que des amas d'étoiles jeunes, n'ayant pas encore connu d'épisode de supernova, puissent être des accélérateurs cosmiques.Pour ce type d'investigation, l'astronomie gamma est aux premières loges puisque contrairement au rayonnement cosmique chargé, ce type de messager céleste n'est pas dévié dans son voyage depuis la source jusqu'à nous.L'objet de ce travail est ainsi d'évaluer la possibilité pour ces amas d'étoiles jeunes, de recycler une partie de l'énergie mécanique transférée au milieu interstellaire dans l'accélération de particules et partant, dans l'émission d'un rayonnement non-thermique. Cette étude propose, à partir d'un spectre d'injection pour des particules chargées (proton et/ou électrons), de modéliser l'émission non-thermique attendue considérant les pertes que celles-ci subissent. Un catalogue d'amas potentiellement prometteurs est dressé ainsi qu'un classement de ceux-ci au regard du flux de gamma attendu. Une analyse des données des télescopes H.E.S.S. est conduite pour un certain nombre d'amas sélectionnés. Ce réseau de télescopes Cherenkov situé en Namibie est le plus performant dans sa catégorie. Il est dédié à l'observation des rayons gamma de très haute énergie.Une analyse des données du Fermi-LAT ont également été effectuées. Il s'agit cette fois d'un satellite dédié à la partie des hautes énergies du rayonnement gamma.Enfin, on contraint les paramètres de notre modèle grâce aux résultats issus de ces analyses.L'expérience H.E.S.S., qui a fonctionné à 4 télescopes dès 2003, est depuis 2012 au tout début de sa deuxième phase consistant en l'ajout d'un cinquième télescope de plus grand diamètre. On montre ici, grâce à des simulations de gerbes, la nécessité pour ce télescope de disposer d'un système de focus permettant l'ajustement de la distance caméra-miroirs conduisant à de meilleures performances (taux de déclenchement, résolution angulaire). / More than one century ago, Victor Hess discovered the cosmical origin of the mysterious ionizing radiation. Yet, nowadays it still has a lot of secrets for us. Roughly below the PeV energy, the best candidates already proposed in 1934 were the supernovae remnants (SNR). These candidates still remain ; in the past we considered isolated SNRs, while today we rather think about SNRs inside big structures as superbubbles. These objects are formed by powerful stellar winds from massive stars combined with several SNRs gathered in a space of some decades or hundreds of parsecs. Observations show that the majority of the SNRs occurs in such regions. The point for us is to know if star clusters or associations of massive stars, not hosting any SNR, could also accelerate particles to very high energies and consequently emit gamma-rays.The gamma-ray astronomy is relevant in order to solve this type of riddle because the Very High Energy photons do not suffer of any deviation due to the Galactic magnetic field. It means that we can get informations from the source itself by detecting the gamma-ray radiation.In our study we assume that a part of the mechanical energy transferred to the interstellar medium can be used to accelerate charged particles, which will emit non-thermal radiations.First we assume a given injection spectrum (for electrons and/or protons), then we model the non-thermal emission expected considering particles losses.We deliver a catalogue of promising clusters and we rank them according to the expected strength of the gamma-ray flux.We conducted the analysis of H.E.S.S. data collected toward some selected clusters. The H.E.S.S. experiment is situated in Namibia and is the most efficient array of Cherenkov telescopes. We also used the Fermi-LAT public data. Fermi is a space-based telescope for High Energy gamma ray.Then we constrain our model with the obtained analysis results.The H.E.S.S. experiment had initially 4 telescopes in operation since 2003. In 2012, the second phase of the experiment started when a fifth larger one was added. We show here that it is relevant for this telescope to use a focus system in order to move the camera and change the distance camera-mirrors. The simulations show that the focus system leads to better performances (trigger rate, angular resolution).

O plasma de quarks e glúons é uma previsão da cromodinâmica quântica e experimentos em aceleradores de alta energia têm encontrado evidências experimentais de sua criação em colisões de íons pesados relativísticos. Uma dessas evidências foi proposta por Matsui e Satz [1] que prevê a supressão de estados de heavy quarkonium na existência deste plasma. Este projeto tem como objetivo obter a seção de choque da produção de no experimento STAR em colisões p+p e d+Au com energia no centro de massa de 200GeV e calcular o fator de modificação nuclear Rab. Para tal, foi necessário reconstruir os através de seu decaimento leptônico. Os subdetectores do STAR utilizados foram o TPC e BEMC. Os valores encontrados para seção de choque foram de 3i=1 (nS)e-e+(nS)p+p= 84 ±9(stat)+18-19(sist)pb e 3i=1 (nS)e-e+(nS)d + Au = 41 ± 4(stat) +7-8(sist)nb para as produções pp2009 e dAu2008, respectivamente. Os valores se encontram compatíveis com os teóricos calculados pelo modelo de evaporação de cor. O Rab experimental vale 1.24 ± 0.18(stat)+0.35 0.38(sist). / The quark and gluon plasma is a prediction of QCD, and high energy experiments have studied evidences of its creation in relativistic heavy ion collisions. One of these evidences was proposed by Matsui and Satz [1] that provides a experimental signature of the creation of the plasma, observing an anomalous supression on the heavy quarkonium production. This project aims to get production cross section in the STAR experiment in collisions p+p and d+Au with energy in the center of mass of 200GeV and calculate the nuclear modification factor Rab. To this end, it was necessary to reconstruct the from his leptonic decay. The subsystems used in this analysis were the TPC, BEMC and the heavy quarkonia trigger system. The values for the cross sections were 3i=1 (nS)e-e+(nS)p+p= 84 ±9(stat)+18-19(sist)pb and 3i=1 (nS)e-e+(nS)d + Au = 41 ± 4(stat) +7-8(sist)nb for pp2009 and dAu2008 productions, respectively. These values are compatible with the theoretical calculated by the color evaporation model. The determined value for the factor Rab was 1.24 ± 0.18(stat)+0.35 0.38(sist).

Orientador: Jun Takahashi / Dissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Fisica Gleb Wataghin / Made available in DSpace on 2018-08-11T10:25:44Z (GMT). No. of bitstreams: 1 Souza_RafaelDerradide_M.pdf: 5190148 bytes, checksum: 9951aed4d9ff0a2b1db393891c1ac465 (MD5) Previous issue date: 2008 / Resumo: Reações nucleares envolvendo núcleos pesados em energia de colisão no limite relativístico são estudadas para conhecer as leis e características da matéria em condições extremas de energia e temperatura. Em uma colisão de núcleos pesados no regime relativístico, milhares de partículas são produzidas. Neste trabalho, estudamos a produção de partículas analisando os dados de colisões de íons pesados relativísticos, medidos pelo experimento STAR do acelerador RHIC, com uma abordagem estatístico-termodinâmica. Usando o formalismo grande-canônico, foram feitos estudos da dependência dos parâmetros termodinâmicos com o volume dos sistemas formados em colisões de íons de ouro ( 197 Au) nas energias de 62,4 e 200 GeV por par de núcleon e colisões de íons de cobre ( 63 Cu) na energia de 200 GeV por par de núcleon. Observou-se que o grau de equilíbrio do setor de estranheza é equivalente entre os sistemas criados em colisões centrais de íons de cobre e os criados em colisões periféricas de íons de ouro na energia de 200 GeV por par de núcleon. Também foi analisada a dependência dos parâmetros termodinâmicos com relação à rapidez das partículas produzidas na reação e os resultados mostraram um forte aumento dos potenciais químicos bariônico e de estranheza para as regiões longitudinais das distribuições de rapidez. Finalmente, foi verificada a dependência dos resultados obtidos em função da energia depositada na reação (ps N N), observando-se uma boa consistência com o comportamento geral de resultados de outros trabalhos encontrados na literatura / Abstract: Nuclear reactions in the relativistic regime are studied to understand the laws and characteristics of nature under extreme conditions of high energy density and temperature. In these collisions, a large number of particles is produced. In this work, we study the particle production mechanism using a statistical thermal approach analysing data measured by the STAR experiment at RHIC. Using a grand-canonical approach a study of the volume dependence of the thermodynamical parameters of the systems formed in gold-gold (197 Au ) collisions at 62.4 and 200 GeV per nucleon pair and copper-copper (63 Cu ) collisions at 200 GeV per nucleon pair was performed. This study showed that the equilibrium is indeed achieved and that, even in the strangeness sector, equilibrium is achieved in the case of most central gold-gold collisions. The dependence of the thermodyna-mical parameters on the particle rapidity was also analysed and the results showed an increase of the baryon and strange chemical potentials with rapidity. Finally, the dependence of the results on the energy deposited in the reaction was verified within a fairly good agreement with the general behaviour of results obtained in similar studies from literature / Mestrado / Física / Mestre em Física

Denna studie undersöker om det är möjligt att införa nåbarhetstestning i en baneditor. Testets syfte är att ersätta manuell testing, det vill säga att bankonstruktören inte ska behöva spela igenom banan för att säkerställa att denne kommer kunna nå alla nåbara positioner.För att kunna utföra studien skapas en enkel baneditor som testplattform. Vidare utförs en jämförande studie av flera alternativa algoritmer för att fastställa vilken som är mest passande för nåbarhetstestning i en baneditor.Resultatet från den jämförande studien visade att A* (A star) var den mest passande algoritmen för funktionen. Huruvida automatisk testning kan ersätta manuell testning är diskutabelt, men resultatet pekar på en ökad effektivitet i tid när det kommer till banbygge. / The following study examines whether it is possible to implement reachability testing in a map editor designed for 2D-platform games. The purpose of reachability testing is to replace manual testing, that being the level designer having to play through the map just to see if the player can reach all supposedly reachable positions in the map.A simple map editor is created to enable the implementation after which we perform a theoretical study in order to determine which algorithm would be best suited for the implementation of the reachability testing.The results comparing algorithms shows that A* (A star) worked best with the function. Whether or not manual testing can be replaced by automatic testing is open for debate, however the results points to an increase in time efficiency when it comes to level design.

Partant du constat de l’extraordinaire pérennité de Katharine Hepburn en tant que star hollywoodienne de premier plan, ce travail se propose d’élucider les raisons de ce succès durable en examinant la réception dont l’actrice a fait l’objet aux États-Unis tout au long de sa carrière. À la croisée des star studies et des études de réception, cette étude articule analyse de sa persona (rôles interprétés à l’écran et à la scène, jeu d’actrice et image médiatique) et des traces de sa réception auprès du public états-unien (critiques de professionnels, courriers de fans, sondages, données de box-office, etc.). Grâce à une approche diachronique, les évolutions de son image et de sa réception sont réinscrites dans un contexte socio-historique en perpétuelle évolution, auquel la star a tenté de s’adapter avec plus ou moins de succès suivant les périodes. L’examen des matériaux extra-filmiques participant à la construction de son image ou témoignant de sa réception permettent d’éclairer sous un nouveau jour les performances de Hepburn, analysées dans leur dimension socio-culturelle, esthétique et actorale. Une attention particulière est portée aux dimensions de genre, de classe et de génération de sa persona. / Acknowledging the extraordinary longevity of Katharine Hepburn as a high-profile Hollywood star, this study seeks to shed light on the reasons behind this lasting success by examining her reception in the United States throughout her career. Combining both star studies and reception studies, this thesis articulates the analysis of her persona (her theater and film roles, her acting and media image) with evidence of her reception by the United States audience (critics, fan letters, polls, box-office figures, etc.). Using a diachronic approach, the evolutions of her image and its reception are incorporated within the framework of a socio-historical context in constant evolution, to which Hepburn tried to adapt with differing success depending on the period. The examination of the extra-filmic materials that contribute to her image or testify to her reception allow us to shed new light on Hepburn’s performances, analyzed from a socio-cultural, aesthetic and acting perspective. Special attention is given to the gender, class and age-related dimensions of her persona.

In this thesis we test and expand our current knowledge of Star Formation Laws (SF laws) in the extreme environment of dwarf irregular galaxies. We focus on the SF characteristics of our 18 galaxies sample, extending current investigations of the Schmidt-Kennicutt law to the low luminosity, low metallicity regime. The Hi data used in this project have been observed, calibrated and imaged according to the LITTLE THINGS Survey prescription to which I brought my own contribution as a member of the team. Apart from high resolution, VLA data in B, C and D array configurations, this project makes use of an extensive set of multi- wavelength data (H , FUV, 24 m, 3.6 m, V-band and K-band). Molecular gas in dwarfs is very difficult to observe, mainly because due to the low metallicity environment, we lose our only molecular tracer, the CO which becomes under luminous. Therefore the gas distribution is represented by Hi gas only. We create our Star Formation Rate (SFR) maps mainly based on FUV maps because our analysis shows that FUV is the SF tracer that allows us the most extensive sampling of the SFR surface density (SFRD) and Hi surface density relation. The main results of our study are: Whereas in spiral galaxies Bigiel et al. (2008) have found a one to one relation between star formation rate and molecular gas and no relation between the SFR and the neutral gas, in a small sample of dwarfs as well as in the outskirts of spiral galaxies Bigiel et al. (2010b) has found that SFRD does correlate with Hi surface density. We confirm the existence of the SFRD vs. Hi surface density relation in dwarf irregular galaxies and a linear fitting through all our data (all 18 galaxies combined) yields a power law relation ΣSFR ∝ Σ1.87±0.3/HI . We find that the interiors of Hi shells, at 400 pc scales, become resolved and show up in SFRD versus Hi surface density plots although within the shell interior we have SFRD values but no Hi surface density related to them. Thus, the points originating from those regions contribute significantly to the increase of the scatter in the plot. We show that by excluding those points the correlation between SFRD and Hi surface density improves between 10% and 20%. Eight of the 18 galaxies in our sample have Hi maxima higher than the 10M pc-2 value found by Bigiel et al. (2008) for spiral galaxies. Krumholz et al. (2011) predicted that the 10M pc-2 threshold is metallicity dependent in galaxies with sub-solar metallicity, however the theoretically predicted values for our galaxies only match the observed Hi maxima in one case (DDO168). We find that metallicity cannot be the only factor setting the Hi to H2 transition. In fact, we find evidence that the higher the interstellar radiation field (ISRF), the higher the Hi maximum is, hence we suggest that the ISRF should also be taken into consideration in predicting the Hi to H2 transition threshold. We find that even tighter than the SFRD vs. Hi surface density relation is the SFRD vs. V-band surface density relation. Unlike the SFRD vs. Hi surface density relation the SFRD vs. V-band surface density relation follows a power law and can be written as follows: ΣSFR ∝ (10^μv)^-0.43±0.03. The SFRD vs. V-band surface density relation suggests that the existing stars also play a role in the formation of the next generation of stars. Within our sample of dwarf galaxies the average pressure per resolution element and the SFRD are in a 1:1 linear relation: ΣSFR ∝ P_h^1.02±0.05. A similar relation has been found by Blitz & Rosolowsky (2006) for the low-pressure regimes of spiral galaxies. In conclusion we find that in the extreme environments of dwarf galaxies the metal deficiency and the lack of the classic SF stimulators (spiral arms, shear motions) do not impede the star forming process. In these galaxies, dust-shielding becomes predominantly self-shielding and there is plenty of Hi available to achieve this additional task. Existing stars assume the role of pressure enhancers, which in turn will stimulate SF without the need of spiral arms or shear motion.

An area in graph theory is graph colouring, which essentially is a labeling of the vertices or edges according to certain constraints. In this thesis we consider star edge colouring, which is a variant of proper edge colouring where we additionally require the graph to have no two-coloured paths or cycles with length 4. The smallest number of colours needed to colour a graph G with a star edge colouring is called the star chromatic index of G and is denoted <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?%5Cchi'_%7Bst%7D(G)" />. This paper proves an upper bound of the star chromatic index of bipartite graphs in terms of the maximum degree; the maximum degree of G is the largest number of edges incident to a single vertex in G. For bipartite graphs Bk with maximum degree <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?k%5Cgeq1" />, the star chromatic index is proven to satisfy<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?%20%5Cchi'_%7Bst%7D(B_k)%20%5Cleq%20k%5E2%20-%20k%20+%201" />. For bipartite graphs <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?B_%7Bk,n%7D" />, where all vertices in one part have degree n, and all vertices in the other part have degree k, it is proven that the star chromatic index satisfies <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?%5Cchi'_%7Bst%7D(Bk,n)%20%5Cleq%20k%5E2%20-2k%20+%20n%20+%201,%20k%20%5Cgeq%20n%20%3E%201" />. We also prove an upper bound for a special case of multipartite graphs, namely <img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?K_%7Bn,1,1,%5Cdots,1%7D" /> with m parts of size one. The star chromatic index of such a graph satisfies<img src="http://www.diva-portal.org/cgi-bin/mimetex.cgi?%5Cchi'_%7Bst%7D(K_%7Bn,1,1,%5Cdots,1%7D)%20%5Cleq%2015%5Clceil%5Cfrac%7Bn%7D%7B8%7D%5Crceil%5Ccdot%5Clceil%5Cfrac%7Bm%7D%7B8%7D%5Crceil%20+%20%5Cfrac%7B1%7D%7B2%7Dm(m-1),%5C,m%20%5Cgeq%205" />. For complete multipartite graphs where m &lt; 5, we prove lower upper bounds than the one above.

[pt] O principal objetivo desta dissertação é estudar modelos de previsão da geração eólica utilizando os dados de cinco parques eólicos, mais precisamente comparar o desempenho dos modelos lineares e não lineares. Utilizando a metodologia do modelo não-linear STAR-TREE (Smooth Transition AutoRegression Tree) e comparando com o modelo linear Box e Jenkins através de medidas estatísticas. Basicamente, o modelo STAR-TREE é uma combinação dos modelos STAR (Smooth Transition AutoRegression) e CART (Classification and Regression Tree), realizando assim uma modelagem em árvore onde a transição entre os regimes é feita de forma suave através da função logística e nos nós terminais são ajustados modelos preditivos. Neste estudo será ajustado nos nós terminais um modelo simples constante e também modelos autorregressivos. / [en] The main objective of this dissertation is to study wind generation forecasting models using data from five wind farms, more accurately compare the performance of linear and nonlinear models. Using the methodology of the nonlinear model STAR-TREE (Smooth Transition Autoregression Tree) and compare with the linear model BoxandJenkins through statistical measures. Basically the model STAR-TREE is a combination of models STAR (Smooth Transition Autoregression) and CART (Classification and Regression Tree), thus creating a modeling tree where the transition between regimes is done smoothly through the logistics function and in the terminal nodes are adjusted predictive models. In this study will fit in the terminal nodes, a simple model of constant and a autoregressive models.

The nature of high-energy gamma-ray emission from Star-Forming Galaxies is of utmost importance for understanding both the origin of Cosmic Rays and the high-energy processes that shape galaxy formation. Observations from the gamma-ray telescope Fermi-LAT have detected gamma-ray emission from a handful of nearby Star-Forming Galaxies. Interestingly, observations of the Small Magellanic Cloud show evidence for a spectral cutoff at energies of approximately 10 GeV. This has raised the question as to whether some Star-Forming Galaxies are unable to contain their Cosmic Ray population. Using the Fermitools to analyse the gamma-ray emission from a selection of bright nearby Star-Forming Galaxies, this study intends to explore the possibility of finding further evidence for exponential cutoffs in the gamma-ray spectrum of Star-Forming Galaxies. The shape of the combined spectrum of the 49 galaxies in the sample was determined using least-square fitting of a single power law, a broken power law and a power law with an exponential cutoff. No evidence of an exponentialcutoff was found and the shape of the spectrum was best described by a broken power law with indices Γ1 = -2.48 ± 0.05 and Γ2 = -0.88 ± 0.09. This is in poor agreement with previous observations, which favour a simple power law with an index in the range -2.2 to -2.4. Interestingly, the single power law, while disfavoured over the broken power law at ~7σ, was best fit with the index Γ = -2.35 ± 0.06, which is surprisingly well in agreement with previous observations. The discrepancy between the results presented here and those found in the literature is interpreted as due to insufficient treatment of background fluctuations and the possible existence of bright sources at the unverified blank sky locations used for modelling the background.

Film music has its roots in late-romantic concert music. A number of composers of so-called “serious music” also composed for the film. And some Golden Age film composers came from the concert-music realm and, once they started their association with Hollywood, continued to pen works for the concert stage too. Film music had to struggle for a long time against the prejudice that saw it as music not to be taken seriously; it was regarded as “neglected art”. Nevertheless, film-music concerts have experienced a blossoming in the recent years. There is a large variety, from programmes that only perform film music in concert halls without any additional element to large-scale events in multi-purpose halls where film music is accompanied by film clips or provides the live accompaniment to entire films. This chapter examines the role of John Williams’s film scores in this context. Are there any special features of Williams’s film music that make it particularly suitable to the concert hall? How does the performance practice of his film music differ in comparison to classical concerts? Are there any pieces that are played more frequently than others, and if so, why?