La gravité quantique à boucles a fourni un cadre d’étude particulièrement bien adapté aux théories de jauge définies sans métrique fixe et invariante sous difféomorphismes. Les excitations fondamentales de cette quantification sont appelées réseaux de spins, et dans le contexte de la relativité générale donnent un sens à la géométrie quantique au niveau canonique. Les mousses de spins constituent une sorte d’intégrale de chemins adaptée aux réseaux de spins, et donc destinée à permettre le calcul des amplitudes de transition entre ces états. Cette quantification est particulièrement efficace pour les théories des champs topologiques, comme Yang-Mills 2d, la gravité 3d ou les théories BF, et des modèles ont aussi été proposés pour la gravité quantique en dimension 4.Nous discutons dans cette thèse différentes méthodes pour l’étude des modèles de mousses de spins.Nous présentons en particulier des relations de récurrence sur les amplitudes de mousses de spins. De manière générique, elles codent des symétries classiques au niveau quantique, et sont susceptible de permettre de faire le lien avec les contraintes hamiltoniennes. De telles relations s’interprètent naturellement en termes de déformations élémentaires sur des structures géométriques discrètes, telles que simplicielles. Une autre méthode intéressante consiste à explorer la façon dont on peut réécrire les modèles de mousses de spins comme des intégrales de chemins pour des systèmes de géométries sur réseau, en s’inspirant à la fois des modèles topologiques et du calcul de Regge. Cela aboutit à une vision très géométrique des modèles, et fournit des actions classiques sur réseau dont on étudie les points stationnaires. / Loop quantum gravity has provided us with a canonical framework especially devised for back-ground independent and diffeomorphism invariant gauge field theories. In this quantization the funda-mental excitations are called spin network states, and in the context of general relativity, they give ameaning to quantum geometry. Spin foams are a sort of path integral for spin network states, supposed to enable the computations of transition amplitudes between these states. The spin foam quantization has proved very efficient for topological field theories, like 2d Yang-Mills, 3d gravity or BF theories. Different models have also been proposed for 4-dimensional quantum gravity.In this PhD manuscript, I discuss several methods to study spin foam models. In particular, I present some recurrence relations on spin foam amplitudes, which generically encode classical symme-tries at the quantum level, and are likely to help fill the gap with the Hamiltonian constraints. These relations can be naturally interpreted in terms of elementary deformations of discrete geometric struc-tures, like simplicial geometries. Another interesting method consists in exploring the way spin foam models can be written as path integrals for systems of geometries on a lattice, taking inspiration from topological models and Regge calculus. This leads to a very geometric view on spin foams, and gives classical action principles which are studied in details.

Depuis 1916, l'étude des Trous Noirs a soulevé des questions intrigantes. Seulement certaines ont été résolues. En effet, nous faisons face à des régimes où s’entremêlent la théorie quantique et l'espace-temps. Les TN comme porte d'entrée pour comprendre la nature quantique de la gravité. Ma thèse a été entièrement dédiée à ce domaine central de la physique théorique, avec pour but la compréhension la plus large possible des débats autour de ces questions. C'est ainsi qu'ont été produits des résultats originaux qui constituent le cœur de ce manuscrit. 1-Les surfaces de volume maximal des TN sont étudiées. Un TN astrophysique terminera sa vie avec une aire planckienne de $10^{-70} m^2$ dissimulant $10^5$ fois le volume de l'univers observable. Ceci peut avoir des conséquences sur la viabilité du "remnant scenario" comme solution au paradoxe de l'information. 2-Le scénario "trou-noir-trou-blanc" est fortement instable. Une modification minimale est proposée pour résoudre ce problème. 3-Une généralisation des quatre lois de la thermodynamique des TN est démontrée pour des cônes de lumière s'intersectant dans un espace de Minkowski. 4-On étudie des espaces conformellement plats où de telles lois acquièrent une interprétation thermodynamique standard. Le plus simple est l'espace-temps de Bertotti-Robinson, connu pour encoder la géométrie proche de l'horizon d'un TN chargé. 5-Pour peu que le bon tenseur énergie-impulsion soit identifié, les équations du champ Einstein-Cartan peuvent être retrouvées comme l'équation d'état d'un équilibre thermodynamique, comme dans le cas original de la RG. Ces résultats contribuent au débat intense sur les questions cruciales posées ci-dessus. / Since 1916 intriguing questions have arisen from the study of Black Holes (BH). Only some of them have been resolved. Indeed, we are faced with regimes where the yet unknown interplay between quantum theory and spacetime unveils. BH physics is a gateway to the quantum nature of gravity. My thesis has been completely devoted to this central domain of theoretical physics, with the guiding aim of understanding in the widest possible manner the debate around those questions. The process has produced original results that constitute the main core of the manuscript. 1- The maximal volume surfaces of evaporating BHs are studied. An astrophysical BH will end its life with an external planckian area $10^{-70} m^2$ hiding $10^5$ times the volume of our observable Universe. This can have consequences on the viability of the “remnant scenario” as solution to the BH information paradox. 2- The “black-hole-to-white-hole scenario” is analyzed. The model is shown to be strongly unstable, and a minimal resolutive modification is proposed. 3- A generalisation of the four laws of BH thermodynamics is proven for intersecting light cones in Minkowski spacetime. 4- Conformally flat spaces where such laws acquire the standard thermodynamical interpretation are studied. The simplest one is the Bertotti-Robinson spacetime, known to encode the near-horizon geometry of a charged BH. 5- It is shown that, if the correct energy-momentum tensor is identified, the Eintein-Cartan’s field equations can be recovered as a thermodynamical equilibrium equation of state just like in the GR original case. Such results contribute to the intense debate on the opening crucial questions.

Neste trabalho estudamos a dinâmica de discos torcidos finos e espessos para compreender melhor a propagação da deformação nestes discos. No caso dos discos finos, estudamos a física do efeito Bardeen-Petterson e aplicamos este modelo para explicar o jato em escalas de parsec e kilo-parsec da galáxia NGC 1275. Encotramos que o efeito Bardeen-Petterson reproduziu muito bem a forma do jato e com isto derivamos os parâmetros do disco como raio, valores das viscosidades azimutal e vertical, lei de potência da densidade superficial e spin do buraco negro. Para uma melhor compreensão da física destes discos, realizamos simulações GRMHD de discos moderadamente finos tanto planos como inclinados para estudar a evolução do ângulo de inclinação entre os momentos angular do buraco negro e do disco de acresção assim como o ângulo de torção que está associado com a precessão do disco. Encontramos que quando o disco de acresção e o buraco negro rotacionam no mesmo sentido, o ângulo de inclinação entre os momentos angular apresentou um comportamento oscilatório na parte interna do disco e permaneceu constante na parte externa em acordo com as previsões teóricas. Já quando o buraco negro rotacina no sentido oposto ao disco de acresção, encontramos pela primeira vez numa simulação GRMHD evidências de alinhamento, ocorrendo um alinhamento de 10\\% do angulo entre os momentos angulares do disco e buraco negro. Além disso, comprovamos pela primeira vez numa simulação GRMHD a não isotropia do stress. Utilizando um modelo semi-analítico, comparamos os resultados de nossas simulações com este modelo, utilizando os dados da simulações de disco plano como entrada e obitivemos os mesmos comportamentos das simulações tanto no caso prógrado quanto no caso retrógrado mostrando que o alinhamento é devido ao regime onda. / In this work we studied the dynamics of twisted thin and thick disks to better understand how the warp propagates in these discs. In the case of thin discs, we studied the physics of the Bardeen-Petterson effect and we applied this model to explain the shape of the jet in both parsec and kilo-parsec scales of the galaxy NGC 1275. We found that the Bardeen-Petterson effect could explain very well the shape of the jet and with that we derived the disc parameters such as its radius, the values of the kinematic azimutal and vertical viscosities, the power-law of the surface density and the spin of the black hole. To better understand the physics of such discs, we have performed GRMHD simulations of moderatelly thin tilted disks to study the evolution of the tilt angle between the angular momentum of the accretion disk and black hole and also the twist angle which is associated with the precession of the disc. We found that when the accretion disc and the black hole are rotating in the same direction, the tilt angle showed an oscillatory behavior in the inner parts of the disk while in the outer parts it remained constant in agreement with the theorical modelos. However, when both rotate in the opposite direction, we found for the very first time in a GRMHD simulation, evidences of alignment of 10\\% of the tilt angle. Besides that, we prove for the first time in a GRMHD simulation that the stress is far from being isotropic. Using a semi-analitic model, we compared the results of our simulations with this model, using the datas of the untilted simulations as inputs and we found the same behaviors found in the simulations even in prograde case as in the retrograde case showing that the alignment is due to bending waves.

A colisão de buracos negros é uma das fontes mais importantes de ondas gravitacionais e, em geral, a emissão anisotrópica da radiação causa um recuo do objeto final. Este cenário já é conhecido há décadas, mas foi somente com o recente avanço na relatividade numérica que as velocidades finais dos objetos radiantes foram computadas com precisão. Os valores encontrados podem ser altos o suficiente para exercerem um importante papel no crescimento de buracos negros super massivos via coleção de galáxias e na abundância de núcleos galáticos ativos contendo buracos negros. Este é um autêntico efeito da não linearidade de Relatividade Geral e esta tese fornece uma nova metodologia estudar alguns aspectos da dinâmica da colisão de buracos negros. Consideramos o horizonte como uma tela canônica que codifica as informações da evolução temporal do espaço-tempo. Com esta hipótese, fenômenos como o anti-kick, isto é, uma súbita desaceleração do sistema antes de atingir a velocidade final, são explicado em termos da dissipação das deformações do horizonte. Estudamos primeiramente o Espaço-tempo de Robinson-Trautman. Uma das solução mais simples das equações de Einstein, esta métrica nos fornece um poderoso modelo para investigar tanto a perda de massa quanto o recuo do objeto final. Mostramos que, quando as configurações iniciais tem simetria especular, a massa do buraco negro remanescente e a energia irradiada são completamente determinadas pela condição inicial. Com isso, obtemos as expressões analíticas dos resultados numéricos obtidos anteriormente na literatura. Além disto, com o auxilio do método espectral de Galerkin, analisamos o regime não linear das equações envolvidas e verificamos que se pode estimar a velocidade de recuo final com boa precisão a partir de medidas da assimetria da condição inicial. Introduzimos na seqüência a curvatura efetiva como uma medida das deformações intrínsecas ao horizonte. Além de considerar as deformações gerais, ela também inclui as diferenças entre os hemisférios norte e sul. No espaço-tempo de Robinson-Trautman, essa quantidade se correlaciona de uma forma injetora com a velocidade final. Para superar algumas limitações dessa solução, aplicamos o mesmo procedimento nos resultados da simulação numérica de uma colisão head-on. Neste caso, a curvatura efetiva, está na realidade, correlacionada com a aceleração do sistema. Refinamentos e generalizações desta técnica são também discutidos e propostos para trabalhos futuros. / Colliding black holes are one of the most important sources of gravitational waves and the anisotropic emission of the radiation generally causes the recoil of the final hole. This scenario has been known for decades, but it is only thanks to the recent progress in numerical relativity that the final velocity have been accurately computed. The values found can be large enough to play an important role in the growth of supermassive black holes via mergers of galaxies and on the number of galaxies containing them. This is a genuine nonlinear effect of general relativity and this thesis provides a new methodology to study some features on the dynamics of the collision. We propose that the horizon is a canonical screen, which encodes he information of its surroundings. With this assumption, phenomena such as the anti-kick, namely the sudden deceleration before reaching the final velocity, are explained in terms of the dissipation of the horizons deformation. We first study the Robinson-Trautman spacetime. One of the simplest solutions of Einsteins equations, it provides us with a powerful toymodel to investigate both the mass loss of the system and the recoil of the final object. We show that, for the case of reflectionsymmetric initial configurations, the mass of the remnant black-hole and the total energy radiated away are completely determined by the initial data, allowing us to obtain analytical expressions for some numerical results that had appeared in the literature. Moreover, by using the Galerkin spectral method to analyze the non-linear regime of the equations involved, we found that the recoil velocity can be estimated with good accuracy from some symmetry measures of the initial data. Then we introduce the effective urvature as a measure of intrinsic deformations on the horizon. Not only does it account for overall deformation, but also for the differences on the north and south hemispheres. In the Robinson-Trautman spacetime, this quantity correlates in an injective way with the final velocity. To overcome some caveats of this solutions, we apply the same procedure to the results given by numerical simulations of a head-on collision. In the case, the effective curvature is actually correlated with the acceleration of the system. Further improvement and generalizations of this technic is also discussed and proposed for future work.

O objeto de estudo desta dissertação é o efeito de criação de partículas pela curvatura sob o escopo de uma teoria de espalhamento, discutindo quando que a interpretação a partir de uma matriz S é tangível e obtendo sua expressão nesses casos. O capítulo de introdução aborda superficialmente conceitos de relatividade geral e de teoria quântica de campos em espaços planos e curvos, necessários para a construção da matriz S. O conteúdo deste capítulo segue as apresentações feitas por Wald, Parker e Birrell em geral, tendo como guia as obras de Bar, Wald e Hawking no que se trata especificamente de relatividade geral, e de Penrose e Rindler no que se trata da estrutura espinorial. A construção da matriz S se dá no capítulo 2, tendo como guia o trabalho de Wald. O capítulo 3 apresenta exemplos que permitem a contextualização da criação de partículas em casos específicos de espaços-tempos em expansão. Este estudo nos permite verificar que as condições que precisam ser satisfeitas em um espaço-tempo globalmente hiperbólico e assintoticamente estacionário para que a formulação da matriz S possa ser feita são que as teorias no passado e futuro distantes devem ser unitariamente equivalentes, que a relação entre as regiões se dá através de transformações de Bogolyubov dadas por operadores limitados definidos em toda a parte e que tais operadores satisfaçam a condição de Hilbert-Schmidt. Nestes casos obtemos uma expressão para a matriz $S$ que descreve a criação de partículas pela curvatura do espaço-tempo para o campo de Klein-Gordon e de Dirac, além de outras relações úteis, como número médio de partículas criadas e probabilidade de se encontrar partículas em determinado modo, o que permite uma analogia com a radiação de corpo negro, passo fundamental para se entender fenômenos de grande interesse na física, como a radiação de Hawking e a criação de partículas no período inflacionário. / This master\'s thesis deals with the effect of particle creation by the curvature of space-time according to the point of view of scattering theory, discussing when such interpretation is possible by means of an S-matrix and obtaining its expression in those cases. The first chapter treats, superficially, some concepts of general relativity and quantum field theory in plane and curved space-times that are imperative to understand the construction of the S-matrix. The subject of this chapter is covered in the work of Wald, Parker, and Birrell, and follows closely the work of Bar, Wald and Hawking, when treats concepts specifically from general relativity, and from Penrose and Rindler, when talking about the spinor structure of space-time. The construction of the S-matrix is made in the second chapter, along the lines of the work of Wald. The third chapter presents some examples that bring some light on the creation of particles in specific cases of expanding space-times. This study let us verify that an S-matrix formulation is tenable, on globally hyperbolic asymptotic stationary curved space-times, if both quantum theories in the distant past and distant future are unitary equivalent, the relation of both regions is made by Bogolyubov transformations by means of everywhere defined bounded operators and that those operators satisfy the Hilbert-Schmidt condition. In those cases we derive the expression of the S-matrix for the Klein-Gordon and Dirac fields. Also we obtain the number of particles created and the probability of find particles in a particular mode, with let one make an analogy with the black body radiation, which is a fundamental step in the direction of understanding interesting phenomena in quantum field theory in curved space-times, like the Hawking radiation and particle creation in the early universe.

Há duas brechas quânticas nos Teoremas da Singularidade em Relatividade Geral: violações das condições clássicas de energia e flutuações quânticas da geometria do espaço-tempo. Nesta dissertação, estudamos a primeira brecha e abordamos os Teoremas da Singularidade através da condição de energia. Revisamos a abordagem algébrica de Teoria Quântica de Campos para o campo de Klein-Gordon e, neste formalismo, revisamos a derivação de uma desigualdade quântica de energia para os estados de Hadamard em espaços-tempos globalmente hiperbólicos. Apesar das desigualdades quânticas de energia não poderem ser aplicadas diretamente nos Teoremas de Singularidade, mostramos que generalizações dos Teoremas de Hawking e Penrose são provadas considerando condições de energia enfraquecidas inspiradas por elas. Assim sendo, os Teoremas de Singularidade continuam valendo se considerarmos efeitos quânticos sutis. A questão de se efeitos de interação ou efeitos de ``backreaction\'\' poderiam quebrá-los ainda está em aberto; há razões para se esperar ambas as respostas. / There are two quantum loopholes in the Singularity Theorems of General Relativity: violations of the classical energy conditions and quantum fluctuations of the spacetime geometry. In this dissertation, we study the first loophole and approach Singularity Theorems through the energy condition. We review the algebraic approach of Quantum Field Theory for the Klein-Gordon field and, within it, we review the derivation of a quantum energy inequality for Hadamard states on globally hyperbolic spacetimes. However quantum energy inequalities cannot be directly applied to Singularity Theorems, we show that generalized Hawking and Penrose Theorems are proven considering weakened energy conditions inspired by them. Hence, Singularity Theorems do hold under subtle quantum effects. The question of whether interaction or backreaction effects could break them is still open; there are reasons to expect both answers.

The present-day interest in gravitational waves, justified by the recent direct detections made by LIGO, is opening the exciting possibility to answer many questions regarding General Relativity in extreme situations. One of these questions is whether black hole are – indeed – described totally by their mass, charge and angular momentum or whether they can have additional long-range hair. This project is concerned with this question. We aim at studying the influence of additional structure on the black hole horizon in the form of long-range hair by studying linearized Einstein equation the solutions when perturbed. More precisely, we will study the Schwarzschild solution, pierced by an infinitely long and thin cosmic string such that the space-time possesses a global deficit angle. Quasi-normal modes are believed to dominate the gravitational wave emission during the ring down phase of an excited black hole that would e.g. be the result of a merger of two ultra-compact objects, therefore linearized perturbations can be considered. With the advent of gravitational wave astronomy the proposed study will be very important when reconstructing the source of the detected gravitational wave signals. / O atual interesse em ondas gravitacionais, justificado pelas detecções diretas feitas pela colaboração LIGO recentemente, está abrindo a excitante possibilidade de responder várias questões a respeito da Relatividade Geral em condições estremas. Uma dessas questões é se buracos negros são – realmente – totalmente discritos apenas por sua massa, carga e momento angular ou se eles podem ter os chamados cabelos de longo alcance adicionais. Nosso projeto se preocupa em responder esta pergunta. Nosso objetivo está em estudar a influência de uma estrutura adicional no horizonte de eventos de um buraco negro através do comportamento da equação linearizada de Einstein quando a solução é perturbada. Mais precisamente, nós estudaremos a solução de Schwarzschild atravessada por uma corda cósmica infinitamente fina, tal corda faz com que o espaço-tempo tenha um hiato angular em seu plano equatorial. Acredita-se que modos quasi-normais dominem a emissão de ondas gravitacionais durante a fase de ringing down de buracos negros excitados que podem, por exemplo, se originar da colisão de objetos ultra compactos, portanto perturbações lineares podem ser consideradas. Com o advento da astronomia através de ondas gravitacionais o estudo proposto será importante para que se possa reconstruir a origem de sinais detectados.

L'objectif de cette thèse est d'étudier différents aspects microscopiques et macroscopiques liés à la présence de superfluidité dans les étoiles à neutrons. Dans un premier temps, nous avons calculé des configurations stationnaires d'étoiles à neutrons superfluides en rotation, en relativité générale, basées sur l'utilisation d'équations d'état réalistes. A l'aide de ces configurations d'équilibre, nous avons ensuite développé un modèle simple de glitch, en relativité générale, vu comme un transfert de moment cinétique entre les neutrons superfluides et les particules chargées constituant l'étoile. Cela nous a permis d'obtenir des temps caractéristiques de montée qui pourront être comparés à de futures observations précises de glitches afin d'apporter de meilleures contraintes sur l'intérieur de ces étoiles. Enfin, nous nous sommes également intéressés à la dynamique des vortex superfluides, en présence de tubes de flux, dans le cas où les protons dans le coeur des étoiles formeraient un supraconducteur de type II. / The aim of this thesis is to study different aspects, both microscopic and macroscopic, associated with the presence of a large amount of superfluid matter inside neutron stars. First, we computed stationary configurations of rotating superfluid neutron stars, in general relativity, using realistic equations of state. Based on these equilibrium configurations, we then developed a simple model of pulsar glitches, in general relativity, seen as angular momentum transfers between the superfluid neutrons and the charged particles composing the star. This enables us to infer spin-up time scales that could be compared with future accurate glitch observations, in order to get some constraints on the interior of neutron stars. Finally, we also focused on the dynamics of superfluid vortex lines, accounting for the presence of fluxtubes, if the protons are forming a type II superconductor in the core of neutron stars.

Some of the brightest and most energetic events in the Universe are associated with the death of stars. These stellar deaths power transient electromagnetic emission which are routinely observed on Earth. This dissertation presents our research on various such transients. Its topics includes, supernova remnants, kilonovae, gamma-ray bursts (GRBs): The "long'' type produced from core-collapse supernovae and the "short'' type associated with neutron star merger events. It also focuses on the disruption of stars by the tidal forces of supermassive black holes i.e., tidal disruption events (TDEs). We model the emission from these transients and compare them to observations in order to draw a number of conclusions and make predictions for future detections. For example, we find that the non-thermal emission from supernovae and kilonovae associated with GRBs can produce long term emission which may be detected as a re-brightening in the overall emission. The sharp cut off observed in some TDE flares can be caused by a pre-existing accretion disk present around a supermassive black hole, which is expected in active galactic nuclei. Our work successfully predicted the nature of the very first electromagnetic detection from a neutron star merger, and was able to reproduce the emission that had been observed for more than one hundred days after the merger. This dissertation also provides frameworks on how the observable features of these transients can be leveraged to probe the properties of the progenitor system and their environment. <br>

In dieser Arbeit beschäftigen wir uns mit zwei Ansätzen zur Quantengravitation (QG), die einander konträr gegenüberstehen: - Erstens mit der Loop Quantum Gravity (LQG), einem eher konservativen Ansatz zur QG, dessen Startpunkt eine Hamiltonsche Formulierung der klassischen Allgemeinen Relativitätstheorie (ART) ist, - zweitens mit der sogenannten Topos-Theorie, angewandt auf die Allgemeine Relativitätstheorie, die die mathematischen Konzepte der Quantentheorie (und möglicherweise auch der ART) radikal umformuliert, was eine immense Redefinition von Konzepten wie Raum, Zeit und Raumzeit zur Folge hätte. Der Grund für die Wahl zweier so verschiedener Ansätzen als Gegenstand dieser Arbeit liegt in der Hoffnung begründet, dass sich diese beiden Ansätze auf einen gemeinsamen Ursprung zurückführen lassen können und somit gegenseitig ergänzen können. Im ersten Teil dieser Arbeit führen wir den allgemeinen Formalismus der LQG ein und gehen dabei insbesondere auf den semiklassischen Sektor der Theorie ein; insbesondere untersuchen wir die semiklassischen Eigenschaften des Volumenoperators. Dieser Operator spielt in der Quantendynamik der LQG eine tragende Rolle, da alle bekannten dynamischen Operatoren auf den Volumenoperator zurückgeführt werden können. Aus diesem Grund ist es auerordentlich wichtig zu überprüfen, dass der klassische Limes des Volumenoperators wirklich mit dem klassischen Volumen übereinstimmt. Anschließend beschäftigen wir uns mit sogenannten Spin Foam Modellen (SFM), welche als ein kovarianter oder Pfadintegralzugang zur kanonischen LQG angesehen werden können. Diese Spin Foam Modelle beruhen auf einer Langrange-Formulierung der LQG mittels einer kovarianten sum-over-histories Beschreibung. Die Entwicklung eines Lagrange-Zuganges zur LQG wurde motiviert durch die Tatsache, dass es in der kanonischen Formulierung der LQG überaus schwierig ist, Übergangsamplituden auszurechnen. Allerdings weichen die Spin Foam Modelle, die wir in dieser Arbeit behandeln in einem entscheidenden Punkt von den bisher in der Literatur diskutierten ab, da wir die Holst-Wirkung Holst [1996] und nicht die Palatini-Wirkung als Ausgangspunkt nehmen. Dies ermöglicht es uns, explizit gewisse Zwangsbedingungen zu lösen, was in den gegenwärtig diskutierten SFM problematisch scheint. Im zweiten Teil dieser Arbeit führen wir in die Topos-Theorie ein und rekapitulieren, wie diese Theorie benutzt werden kann, um die Quantentheorie derart umzuformulieren, dass eine konsistente Quanten-Logik definiert werden kann. Darüber hinaus definieren wir auch eine Topos-Beschreibung der Quantentheorie in der sum-over-histories Formulierung. Unser Ansatz entscheidet sich vom gegenwärtigen consistent-histories Ansatz vor allem dadurch, dass das Konzept der konsistenten Menge (eine Menge von Historien, die nicht mit sich selbst interferieren) keine zentrale Rolle spielt, während es in letzterem grundlegend ist. Diese Tatsache bietet einen interessanten Ausgangspunkt, da eine der Hauptschwierigkeiten im consistent-histories Ansatz darin besteht, die richtige konsistente Menge der Propositionen von Historien zu finden: Im allgemeinen gibt es viele solcher Mengen, und die meisten davon sind nicht miteinander kompatibel. Wir zeigen, dass in unserer Topos-Beschreibung der sum-over-histories Quantentheorie jeder Proposition von Historien Wahrheitswerte zugeteilt werden können; daher ist das Konzept einer konsistenten Menge von Propositionen redundant. Dies bedeutet, dass es im Rahmen einer Quantengravitationstheorie möglich sein könnte, jeder Proposition von vierdimensionalen Metriken (welche als allgemein relativistisches Analogon einer Historie angesehen werden können) einen Wahrheitswert zuzuweisen. / One of the main challenges in theoretical physics over the last five decades has been to reconcile quantum mechanics with general relativity into a theory of quantum gravity. However, such a theory has been proved to be hard to attain due to i) conceptual difficulties present in both the component theories (General Relativity (GR) and Quantum Theory); ii) lack of experimental evidence, since the regimes at which quantum gravity is expected to be applicable are far beyond the range of conceivable experiments. Despite these difficulties, various approaches for a theory of Quantum Gravity have been developed. In this thesis we focus on two such approaches: Loop Quantum Gravity and the Topos theoretic approach. The choice fell on these approaches because, although they both reject the Copenhagen interpretation of quantum theory, their underpinning philosophical approach to formulating a quantum theory of gravity are radically different. In particular LQG is a rather conservative scheme, inheriting all the formalism of both GR and Quantum Theory, as it tries to bring to its logical extreme consequences the possibility of combining the two. On the other hand, the Topos approach involves the idea that a radical change of perspective is needed in order to solve the problem of quantum gravity, especially in regard to the fundamental concepts of `space'' and `time''. Given the partial successes of both approaches, the hope is that it might be possible to find a common ground in which each approach can enrich the other.