Orientador: Jose Augusto Chinellato / Tese (doutorado) - Universidade Estadual de Campinas, Instituto de Fisica Gleb Wataghin / Made available in DSpace on 2018-08-11T05:35:22Z (GMT). No. of bitstreams: 1 Catalani_Fernando_D.pdf: 3151550 bytes, checksum: e2bbe39231b08bdb8fdcd358452d30f5 (MD5) Previous issue date: 2008 / Resumo: Essa tese tinha como objetivo estudar o perfil longitudinal de chuveiros atmosféricos extensos de forma completa. Nós simulamos chuveiros atmosféricos utilizando o programa CORSIKA para diferentes primários e energias acima de 10 17 e V e procuramos relações entre vários parâmetros extraídos do perfil longitudinal, como Xmax, X0, Xmax - X0, FWHM entre outros. Utilizamos os modelos de interação hadrônica QGSJET01 e SIBYLL2.1 nesses estudos. Um resultado obtido foi a contribuição de diferentes componentes de um chuveiro atmosférico no depósito de energia na atmosfera, para diferentes ângulos, primários e modelos de interação hadrônica. Calculamos, pela primeira vez, explicitamente as quantidades de energia calorimétrica e energia perdida que são necessárias para a recosntrução da energia do primário. Pudemos, então, parametrizar a fração de energia perdida em termos da energia calorimétrica e da energia do primário. Essa parametrização varia menos de 1 % com o ângulo zenital e com o nível de observação. Já a dependência com o primário é menor que 5 % e com o modelo de interação hadrônica é menor que 2 %.Calculamos como menor que 3 % o erro sistemático de corrigir a energia perdida usando uma parametrização mista de 50 % de chuveiros de ferro e 50 % chuveiros de próton. Aplicamos métodos estatísticos no estudo da composição de raios cósmicos. Como resultado, propomos a utilização de vários parâmetros do perfil longitudinal como Xmax, Nmax, Sigma, Assimetria, Skewness and Kurtose. Através do método de análise de componentes principais (PCA) nós estudamos a relevência de cada um desses parâmetros na caracterização do perfil longitudinal. Aplicamos, então, a análise de discriminantes lineares (LDA) para encontrar uma combinação linear dos parâmetros usados que melhor classifique um chuveiro como sendo originado por próton, ferro e fótons. Mostramos que LDA permite uma melhor separação entre chuveiros de hádrons e fótons e entre chuveiros de prótons e ferro que métodos baseados apenas na medida de Xmax / Abstract: The aim of this thesis was to study in a thoroughly way the longitudinal profile of air showers. We simulated air showers for different primaries and energies with the CORSIKA program and searched for relations between several parameters extracted from longitudinal profile, like Xsub>max, X0, Xmax-X0, FWHM and others. Hadronic interaction models QGSJET01 and SiBYLL2.1 were used in these studies. One result was the contribution for different components of an air shower to the energy deposit in the atmosphere, considering different angles, primary particles and hadronic interaction models was studied. We calculated, for the first time, the amounts of calorimetric energy and missing energy which are essential to reconstruct the primary energy. Thus, we could parameterize the fraction of missing energy in terms of the primary energy as a function of calorimetric energy. This parametrization varies less than 1% with angle and observation level. We showed that the dependence with primary mass is less than 5 % and with hadronic interaction model is below 2%. Using a parametrization with a mixture of 50 % of proton and 50 % iron showers at 45° to correct the missing energy the systematic error found was less than 3 %. Finally, we applied statistical methods in the composition studies of air showers. As a result, we propose the utilization of several features of air shower longitudinal profiles such as Xmax, Nmax, Sigma, Asymmetry, Skewness and Kurtosis. First we studied the relevance of each parameter for the overall shower features using principal component analysis (PCA). Then, we applied linear discriminant analysis (LDA) to find a linear combination of the shower parameters that best classifies a shower as an iron, proton or photon originated shower. We showed that LDA provides a better separation between iron and proton showers than using only Xmax-based methods / Doutorado / Física das Particulas Elementares e Campos / Doutor em Ciências

Há várias evidências experimentais da existência de matéria escura no universo. Apesar destas evidências, pouco se sabe sobre sua constituição, sabendo-se apenas que interage gravitacionalmente, mas não eletromagneticamente. Neste projeto, investigamos a possibilidade da matéria escura ser composta por partículas supermassivas e fortemente interagentes (Simpzillas). Para isto determinamos o sinal que deve ser deixado no telescópio IceCube por neutrinos resultantes de aniquilações de matéria escura no Sol. Após determinarmos o espectro de neutrinos no centro do Sol, simulamos sua propagação até a superfície, depois até a Terra e através da Terra até o detector. Comparamos então estes resultados com os fornecidos pelo IceCube. Esta comparação permite testar uma região do espaço de fase massa versus seção de choque previamente não-excluída por outros tipos de experiência que não telescópios de neutrinos. Como resultado, concluímos que partículas supermassivas e fortemente interagentes não podem constituir a matéria escura. / There are many experimental evidences for the existence of dark matter in the universe. Despite these evidences, there is no knowledge about its constitution other than the fact that it interacts gravitationally but not electromagnetically. In this project, we investigate the possibility that dark matter is composed of strongly interacting massive particles (Simpzillas). We determine the expected signal in the IceCube telescope from Simpzilla annihilation in the center of the Sun. We first determine the neutrino spectrum in the core of the Sun. We then simulate its propagation through both the Sun and Earth, and finally the rate of neutrinos at the detector. A comparison of these results to the ones published by the IceCube collaboration covers a large region of the yet not excluded regions of the mass versus cross-section phase space. As a result, the possibility of Simpzillas composing the dark matter is ruled out.

A hipótese de que a matéria estranha de quarks (um plasma composto por quarks up, down e strange em quantidades aproximadamente iguais) é estável `a pressão nula vem sendo considerada há mais de vinte anos, tanto teoricamente quanto em experimentos específicos para sua eventual detecção. Se a matéria estranha é de fato estável, então poderia haver importantes implicações para a Astrofísica. Entre as mais estimulantes destas implicações está a possibilidade de conversão da matéria nuclear ordinária em matéria estranha no interior das estrelas de nêutrons devido ás altíssimas densidades ali encontradas. Processos tais como coalescência em binárias de estrelas de nêutrons e as próprias supernovas, eventos responsáveis pelo nascimento destas estrelas, poderiam ejetar estruturas finitas de matéria estranha, chamadas strangelets (equivalentes aos núcleos), no meio interestelar. Desta forma, strangelets estariam presentes entre os primários de raios cósmicos e seriam sujeitas a processos elementares análogos aos núcleos ordinários. Nesta Tese, as strangelets são estudadas desde os prováveis sítios para sua produção astrofísica, passando por interações com a matéria do meio interestelar, ate a chegada ás imediações terrestres. Estima-se o fluxo de strangelets de baixa energia que poderia ser mantido aprisionado na magnetosfera da Terra, bem como são estudados os processos de suas interações com componentes da atmosfera, com vistas às assinaturas observacionais então resultantes. Desta forma, são determinadas as características relevantes para a identificação destes exóticos por experimentos que testam o fluxo de raios cósmicos, ajudando na melhor compreensão das propriedades da matéria nuclear em alta densidade bariônica e baixa temperatura. / The strange quark matter hypothesis, which states that a plasma composed of quarks up, down and strange in roughly equal amounts is absolutely stable at zero pressure, has been studied for more than twenty years, both theoretically and during searches for its detection in specific experiments. If strange quark matter is indeed stable, then there could be important implications for the field of Astrophysics. Among the most stimulating ones is the possibility of conversion of ordinary nuclear matter in strange quark matter in the interior of neutron stars due to the extremely high densities reached in the core of these compact objects. Processes such as the merger in neutron star binaries systems and supernovae themselves, responsible for the birth of these stars, may eject lumps of strange quark matter, termed strangelets, in the interstellar medium. In this way, strangelets may be present among the cosmic ray flux and be subjected to elementary processes much in the same way as ordinary nuclei. In this Thesis, strangelets are studied from their likely astrophysical production sites, passing through the interstellar medium until they reach the Earth neighborhood. Estimates of the low energy flux of strangelets that could be trapped in the terrestrial magnetosphere are given. Also, the interaction of these particles with components in the Earth atmosphere are studied with the aim of providing better understanding of the resulting observational signatures. It allows the determination of the relevant characteristics for the identification of these exotics by experiments testing the cosmic ray flux, helping to better understand the properties of nuclear matter at high densities and low temperatures.

Orientadores: José Pissolato Filho, Pierre Kaufmann / Tese (doutorado) - Universidade Estadual de Campinas, Faculdade de Engenharia Eletrica e de Computação / Made available in DSpace on 2018-08-23T01:41:59Z (GMT). No. of bitstreams: 1 Duro_MagdaAparecidaSalgueiro_D.pdf: 3861523 bytes, checksum: f5896319d2a3653a7903f977210f3ac1 (MD5) Previous issue date: 2013 / Resumo: A atual dependência da sociedade aos diversos sistemas tecnológicos em funcionamento na Terra traz uma constante preocupação pela sua vulnerabilidade a fatores menos conhecidos. As possíveis falhas no fornecimento de energia elétrica podem ocasionar transtornos de grande impacto às comunidades podendo acarretar perdas financeiras expressivas. Diversos fatores podem ocasionar falhas nas linhas de transmissão, entre eles, os fatores climáticos. Nesse contexto, são pouco conhecidas as influências qualitativas de distintos fatores, destacando-se os efeitos do denominado clima espacial. Há indicações que o clima espacial influencia a alta atmosfera terrestre, com repercussão no clima bem como em sistemas de engenharia em operação na Terra. As redes de transmissão de alta tensão representam um grande circuito elétrico pouco acima do solo sujeito a uma série de sobrecargas temporárias de vários tipos, algumas das quais podem levar a falhas. Algumas destas falhas podem estar relacionadas ao ambiente geofísico. Neste trabalho foi analisada uma base de dados sem precedentes de falhas em linhas de transmissão por um longo período (nove anos) numa grande malha localizada no Estado de São Paulo (sudeste do Brasil). O período estudado (1998-2006) compreende uma significativa fração do ciclo de atividade solar 23. A concessionária responsável (ISA.CTEEP) pela operação das linhas estudadas classifica as falhas em noventa e cinco tipos distintos de causas possíveis, sendo que a maior parte está relacionada às descargas atmosféricas. Este estudo está relacionado aos desligamentos devido às descargas atmosféricas, em duas redes de alta voltagem da companhia, de 138 kV e de 440 kV. No período estudado, estes desligamentos correspondem a 1.957 (42,80%) num total de 4.572 para a linha de 138 kV e de 170 (22,28%) sobre 763 para a linha de 440 kV. Equivale a menos de um a cada dez mil do número total de descargas atmosféricas ocorridas na mesma área, o que demonstra alta resiliência das redes de potência em relação aos raios. Durante a época das chuvas, há uma maior concentração de desligamentos. Para todo o período estudado houve redução de 67% e 77% no número de desligamentos devido às descargas atmosféricas, para as linhas de 138 kV e 440 kV, respectivamente, havendo uma boa correspondência com a redução do número de manchas solares. Nenhuma correlação foi encontrada em relação às atividades geomagnéticas caracterizadas pelo índice planetário (Kp) e pelas grandes tempestades (Dst) tanto em longos quanto em curtos prazos. Uma explicação sugerida associa a diminuição da atividade solar ao aumento da condutividade na atmosfera causada pelo maior fluxo de raios cósmicos. Consequentemente poderá ocorrer uma redução do limiar de voltagem necessário para produzir descargas atmosféricas para provocar desligamentos nas redes de alta voltagem. O circuito elétrico global descrito pelo acoplamento ionosfera-terra (a eletrosfera) exerce um papel importante para explicar a redução dos desligamentos. Com o aumento da condutividade atmosférica as descargas são menos potentes, resultando em menor número de desligamentos com o decréscimo do ciclo solar / Abstract: The current society dependence on the operating technological systems on the Earth brings a permanent concern for their vulnerability to not well known factors. Possible failures in electricity supply can cause inconveniences with large impact to the communities, which may cause significant financial losses. Different factors can cause failures in the transmission networks, including, climate factors. In this context, the influences of various qualitative factors, especially the effects of space weather are not well known. There are indications that space weather affects the upper atmosphere, with repercussions on the climate as well as in engineering systems in operation on Earth. High-voltage transmission networks represent large electrical circuits just above the ground which are subjected to a number of transient overcharges of various kinds, some of which may lead to failures. Some failures might be related to anomalies of the geophysical environment. In the present study we analyze a database consisting in a one unprecedented long series of transmission grid failures (nine years) on high-voltage networks located in São Paulo state (southeastern Brazil). The studied period (1998-2006) includes an important fraction of the solar activity cycle 23. The company responsible by the power grid operator (ISA.CTEEP) classifies causes in ninety-five distinct failure classes to explain the transmission grid shut downs. Most of the failures were attributed to atmospheric discharges. We have studied the failures attributed to atmospheric discharge, in the two power grids of the company, 138 kV and 440 kV. The failures attributed to atmospheric discharge correspond to 1.957 (42.80%) for a total 4.572 at 138 kV and to 170 (22.8%) out of 763 at 440 kV. They correspond to less than one ten thousandth of the actual number of atmospheric discharges recorded in the same area, demonstrating the grid's high resilience to breakdowns due to lightning. A clear concentration of failures in the region's thunderstorm season has been found. A significant 67% and 77% reduction in the number of failure rates has been found for the 138 and 440 kV grids, respectively, for the period studied, in good correspondence with the decay in the sunspot numbers. No obvious correlation was found between power failures and geomagnetic activity, represented by (Kp) the planetary index or major geomagnetic storms (Dst) in the period, either on short or on long time scales. One suggested explanation associates the decrease in solar activity to the increased conductivity in the atmosphere caused by increase cosmic ray flux. Consequently there may be a reduction in the threshold voltage necessary to produce discharge atmospheric to cause failures in high-voltage grids. The global electric circuit described by the ionosphere-ground coupling (the electrosphere), plays an important role in explaining the reduction the failures. With increase in conductivity atmospheric discharges are less potent, resulting in fewer failures with the decreasing solar cycle / Doutorado / Energia Eletrica / Doutor em Engenharia Elétrica

The dynamics of the solar corona are dominated by the magnetic field which creates its structure. The magnetic field in most of the corona is ‘frozen’ to the plasma very effectively. The exception is in small localised regions of intense current concentrations where the magnetic field can slip through the plasma and a restructuring of the magnetic field can occur. This process is known as magnetic reconnection and is believed to be responsible for a wide variety of phenomena in the corona, from the rapid energy release of solar flares to the heating of the high-temperature corona. The coronal field itself is three-dimensional (3D), but much of our understanding of reconnection has been developed through two-dimensional (2D) models. This thesis describes several models for fully 3D reconnection, with both kinematic and fully dynamic models presented. The reconnective behaviour is shown to be fundamentally different in many respects from the 2D case. In addition a numerical experiment is described which examines the reconnection process in coronal magnetic flux tubes whose photospheric footpoints are spun, one type of motion observed to occur on the Sun. The large-scale coronal field itself is thought to be generated by a magnetohydrodynamic dynamo operating in the solar interior. Although the dynamo effect itself is not usually associated with reconnection, since the essential element of the problem is to account for the presence of large-scale fields, reconnection is essential for the restructuring of the amplified small-scale flux. Here we examine some simple models of the solar-dynamo process, taking advantage of their simplicity to make a full exploration of their behaviour in a variety of parameter regimes. A wide variety of dynamic behaviour is found in each of the models, including aperiodic modulation of cyclic solutions and intermittency that strongly resembles the historic record of solar magnetic activity.

Cette étude s’inscrit dans le domaine de la microélectronique. Elle consiste à étudier l’impact de la morphologie 3D du dépôt d’énergie sur la modélisation des événements singuliers (SEE) induits par les muons atmosphériques. La démarche a consisté dans un premier temps à modéliser le dépôt d’énergie induits par des protons dans des volumes nanométriques. Pour cela, le code Monte-Carlo GEANT4 a permis de simuler et de stocker dans une base de données, les caractéristiques des traces des dépôts d’énergie des protons. Une fois la démarche validée pour les protons, des simulations du dépôt d’énergie induit par des muons ont été réalisées. Une caméra CCD a été utilisée afin de réaliser des mesures de l’environnement radiatif atmosphérique et de contraindre la modélisation des dépôts d’énergie induits par les muons. Cette étude met en évidence et quantifie l’apport de considérer la distribution radiale du dépôt d’énergie induit par des protons pour des volumes nanométriques, dans les calculs de prédiction des SEE. En revanche, l’étude montre que la considération de la distribution radiale du dépôt d’énergie induit par des muons dans des volumes nanométriques a un impact négligeable sur la modélisation des SEE. Il serait intéressant de réaliser des mesures du dépôt d’énergie induit par des muons dans des technologies nanométriques sous accélérateur. Cela permettrait d’apporter des données expérimentales encore inexistantes, nécessaires au développement de nouveaux modèles physiques plus précis sur la modélisationdu dépôt d’énergie induit par des muons. / This study concerns the domain of the microelectronics. It consists in the studyof the impact of the 3D morphology of the energy deposit on the Single EventEffect (SEE) modeling, induced by atmospheric muons. Over a first phase, theapproach has consisted in the modeling of the energy deposit induced by protonsin nanometric volumes. For that purpose the use of the Monte Carlo code GEANT4has allowed to simulate and stock in a database the tracks characteristics of theenergy deposit induced by protons. Once the approach validated for the protons,simulations of the energy deposit induced by muons have been realized. A CCDcamera has been used in order to measure the radiative atmospheric environmentand to constrain the modeling of the energy deposit induced by muons. This studyhighlights and quantify the contribution of the radial distribution of the energydeposit incuced by protons in nanometric volumes for the SEE prediction. On theother hand, the study shows that the contribution of the radial distribution of theenergy deposit induced by muons in nanometric volumes has a negligeable impacton the SEE modeling. It will be interesting to realize measurements of the energydeposit induced by muons in nanometric technologies under accelerator. This willallow to bring experimental data still nonexistant necessary to the developpmentof new physical models more accurate on the modelization of the energy depositinduced by muons.

This thesis represents the ontological model for the Time Aspects for a Healthcare Organization. It provides information about activities which take place at different interval of time at Ryhov Hospital. These activities are series of actions which may be happen in predefined sequence and at predefined times or may be happen at any time in a General ward or in Emergency ward of a Ryhov Hospital. For achieving above mentioned objective, our supervisor conducts a workshop at the start of thesis. In this workshop, the domain experts explain the main idea of ward activities. From this workshop; the author got a lot of knowledge about activities and time aspects. After this, the author start literature review for achieving valuable knowledge about ward activities, time aspects and also methodology steps which are essentials for ontological model. After developing ontological model for Time Aspects, our supervisor also conducts a second workshop. In this workshop, the author presents the model for evaluation purpose.

Le but de l'expérience EDELWEISS est la détection directe de matière noire sousforme de WIMPs, par l'étude de leur diffusion élastique sur les noyaux de germanium des détecteurs bolomètriques. Le plus problématique des bruits de fond provient des neutrons pouvant mimer l'interaction d'un WIMP dans un détecteur. Ces neutrons sont notamment produits par les rares muons cosmiques de haute énergie qui atteignent le laboratoire souterrain malgré les 4800 m w.e. de roche. Les muons résiduels sont détectés par un système veto de 46 modules de scintillateur plastique entourant l'expérience, qui permet de rejeter la plupart du bruit de fond associé. La détermination précise du bruit de fond neutron résiduel induit par ces muons dans EDELWEISS-III, essentielle pour l'identification des WIMPs, est le but de cette thèse. Le taux de bruit de fond dépend de la géométrie de l'expérience ainsi que des matériaux utilisés, qui ont subi d'importantes modifications depuis EDELWEISS-II. Des simulations GEANT4 du passage des muons dans la nouvelle géométrie ont été réalisées afin d'extraire le taux d'événements induits par les muons dans les bolomètres. Ce taux est en bon accord avec le taux mesuré extrait des données du Run308. En parallèle, une limite inférieure sur l'efficacité du veto muon a été extraite à partir des données bolomètres. Une nouvelle méthode basée sur l'utilisation d'une source d'AmBe a été développée afin d'extraire l'efficacité de chaque module de la simulation. À partir de ces résultats, il a été montré que le bruit de fond attendu est négligeable pour la recherche de WIMPs avec les données du Run308 et ne limitera pas la sensibilité future d'EDELWEISS-III / The aim of the EDELWEISS-III experiment is to detect the elastic scattering of WIMPs from the galactic dark matter halo on germanium bolometers. The most problematic background arises from neutrons, which can mimic a WIMP interaction in a detector. Neutrons are notably induced by high energy cosmic ray muons reaching the underground laboratory despite the 4800 m w.e. of rock overburdened. Remaining muons are tagged using an active muon-veto system of 46 plastic scintillator modules surrounding the experiment, which allows to reject most of the associated background. The goal of this thesis was to give a precise estimation of the irreducible muon-induced neutron background, needed to identify a potential WIMP signal. The expected background depends on the geometry of the experiment as well as on the used materials, both strongly modified since EDELWEISS-II. Geant4-based simulations of muons through the modified geometry were performed to derive the rate of events induced by muons in the bolometer array. This rate has been shown to be in good agreement with the measured one extracted from the Run308 data. In parallel, a lower limit on the muon-veto efficiency was derived using bolometer data only. A new method based on an AmBe source was developed to extract precisely the detection efficiency of individual modules from the simulation. From these results, it was shown that the expected background is negligible for the WIMP search analyses performed with the Run308 data and won't limit the future sensitivity of the EDELWEISS-III experiment

SALT HRS (Southern African Large Telescope High Resolution Échelle Spectrograph) is a high-resolution, high-efficiency spectrograph for the 11m SALT telescope in Sutherland, South Africa. The initial optical design work was performed at the University of Canterbury, New Zealand. Revisions to the concept, the mechanical design, manufacture, assembly and testing have been handled by the Centre for Advanced Instrumentation, at Durham University in the United Kingdom. SALT HRS is a fibre-fed echelle grating spectrograph with four operational modes: low-, medium- and high-resolution and high-stability modes, having spectral resolutions of R ≈16000, 37000, 67000 and 67000 respectively over a wavelength range of 370-890nm. The instrument is of a dual channel, ‘white pupil’ design, in which the primary mirror acts to collimate light onto a single R4 echelle grating, and also to focus dispersed light to an intermediate focus. A dichroic beam-splitter separates the dispersed light into two separate spectral channels. Spherical pupil mirrors transfer the separated beams via a fold mirror to two wavelength-specific volume-phase holographic gratings (VPHGs) used as cross-dispersers. Cross-dispersed spectra are then imaged by two fully dioptric camera systems onto optimized CCD detectors. This thesis presents the results of the laboratory testing and specification of several critical sub-systems of SALT HRS, as well as the development of key software tools for the design verification and operation at the telescope. In Chapter 1 we first review the technical development of high-resolution spectroscopy and its specific implementation in SALT HRS. In Chapter 2 we develop a comprehensive throughput model of the entire system based on a combination of as-built performance and specific throughput measurements in the laboratory. This is used to make some specific predictions for the on-sky performance of SALT HRS and the magnitude limits for science targets. We also present a graphical exposure time calculator based on these measurements which can be used by an astronomer to plan their observations with SALT HRS. Chapter 3 contains a detailed treatise on the optical fibre system of SALT HRS. Considerations for the use of optical fibres in astronomy are provided, as are details of an optional double scrambler, and the various instrument fibre modes. Extensive measurements of focal ratio degradation (FRD) are also presented, with testing of input beam speed; wavelength; fibre bending; variable pupil mirror illumination; and vacuum tank pressure dependency. The systems for fibre management are reviewed, as is the fibre bundle assembly process. Testing of two further sub-systems is described in Chapter 4. Firstly the long-term stability of the mirror mounting mechanisms is determined. The advantages of cross-dispersion of echelle spectra using volume-phase holographic gratings are then discussed, and the results of diffraction efficiency measurements are given for both red and blue channel gratings. Modern CCD technologies are examined in Chapter 5, and the blue detector is experimentally characterized using photon transfer and quantum efficiency curves. It is also used for an investigation into cosmic ray events in CCDs. Results from shielding the detector using lead are described, as is an attempt to distinguish the source of the events based on their morphology. Finally, Chapter 6 deals with the handling of data produced by SALT HRS. Methods of wavelength calibration of the spectra are discussed, including the use of Thorium-Argon lamps and an iodine absorption cell. The implementation of a Python based quick-look data reduction pipeline is reviewed, with a description of the processes performed. A summary of the thesis is given in Chapter 7.

This project aims to study general relativity to the extent to understand the occurrence and behaviors of closed timelike curves (CTCs) in several exact solutions of Einstein’s field equations. The rotating black hole solution, the Gödel universe and the cosmic string solutions are studied in detail to show how CTCs arise in these spacetimes. The chronology-violationing paradoxes and other unphysical aspects of CTCs are discussed. The spacetimes where CTCs arise possess properties which are argumented to be unphysical, such as lack of asymptotic flatness and being innite models. With quantum computational networks it is possible to resolve the paradoxes which CTCs evoke. With all these attempts of resolving CTCs, our conclusion is that CTCs exist quantum mechanically, but there is a mechanism which inhibits them to be detected classically. / Detta projekt åsyftar att studera allmän relativitet i den grad att kunna förstå uppkomsten och företeelsen av tidsliknande slutna kurvor (CTC) i några exakta lösningar till Einsteins ekvationer. Dessa lösningar inkluderar Gödel universen, kosmiska strängar och det roterande svarta hålet, där CTC studeras i mer detalj. CTC är kronologi-kränkande företeelser och paradoxen som uppstår presenteras, samt de argument som ligger till grund till att CTC inte är fysikaliskt verkliga objekt. De tidrum där CTC uppkommer delar gemensamma egenskaper som anses ofysikaliska, som att vara icke asymptotiskt platta tidrum, samt att vara oändliga modeller. Med kvantinformatiska nätverk kan CTC illustreras och de klassiska kronologi-paradoxen kan rättas ut. Slutsatsen är att CTC existerar kvantmekaniskt, men det fnns en mekanism i verkligheten som förhindrar dessa att bli detekterade klassiskt.