Depuis sa formulation au début du 20ème siècle, la théorie de la Relativité Générale a été vérifiée avec une précision sans cesse croissante. Cette théorie prédit, entre autre, l'existence d'ondes gravitationnelles qui restent à ce jour inobservées, et ce malgré de nombreuses tentatives de détections. Ces ondes sont caractérisées par leur absence de masse. Une des questions qui se pose alors est de savoir si cette absence de masse est une condition nécessaire pour que théorie et observations concordent. Pour répondre à cette question, il est indispensable d'étudier les différents aspects des théories décrivant des ondes gravitationnelles massives. Au-delà de cet intérêt purement théorique, l'étude de ces théories est, entre autre, motivée par de récentes observations cosmologiques. Celles-ci indiquent que l'accord entre la Relativité Générale et les observations n'est possible que si on suppose l'existence de matière et d'énergie noires. Cette thèse est dédiée à une classe de théories décrivant des ondes gravitationnelles massives. Dans un premier temps, nous résumons les différents problèmes qui surgissent lorsqu'on tente de donner une masse aux ondes gravitationnelles. Ensuite, nous introduisons une classe de modèles et étudions certaines de leurs caractéristiques. Le premier aspect étudié concerne l'existence d'une interaction de type instantanée. De telles interactions sont possibles étant donné que l'invariance de Lorentz est spontanément brisée dans les modèles considérés. Celles-ci sont dès lors discutées et un exemple concret est fourni. La présence d'une interaction instantanée dans ces modèles a une conséquence directe sur les solutions "trous noirs" des équations du champ. En effet, on s'attend à ce que l'interaction instantanée puisse propager de l'information à l'extérieur d'un trou noir, ce qui entraînerait une modification de ces solutions par rapport à celles de la Relativité Générale. Cette supposition est confirmée par les solutions "trous noirs" obtenues dans cette thèse. Celles-ci peuvent soit imiter une certaine quantité de matière noire, soit conduire à un champ gravitationnel répulsif. Finalement, les mécanismes de formation des grandes structures de l'Univers (galaxies, amas de galaxies, ... ) sont étudiés pour les théories considérées. Cette dernière discussion démontre que ces modèles reproduisent le comportement prévu par la Relativité Générale et sont, par conséquent, en accord avec les observations.

In recent years, there has been an upsurge in interest in three-dimensional theories of gravity. In particular, two theories of massive gravity in three dimensions hold strong promise in the search for fully consistent theories of quantum gravity, an understanding of which will shed light on the problems of quantum gravity in four dimensions. One of these theories is the “old” third-order theory of topologically massive gravity (TMG) and the other one is a “new” fourth-order theory of massive gravity (NMG). Despite this increase in research activity, the problem of finding and classifying solutions of TMG and NMG remains a wide open area of research. In this thesis, we provide explicit new solutions of massive gravity in three dimensions and suggest future directions of research. These solutions belong to the Kundt class of spacetimes. A systematic analysis of the Kundt solutions with constant scalar polynomial curvature invariants provides a glimpse of the structure of the spaces of solutions of the two theories of massive gravity. We also find explicit solutions of topologically massive gravity whose scalar polynomial curvature invariants are not all constant, and these are the first such solutions. A number of properties of Kundt solutions of TMG and NMG, such as an identification of solutions which lie at the intersection of the full nonlinear and linearized theories, are also derived. / text

General relativity describes gravity in terms of an interacting massless spin-2 field - the graviton. This 100-year-old theory has been spectacularly successful in explaining observations. However, theoretical exploration and the cosmological constant problem motivate the study of alternative theories of gravity. Recently, there has been great progress in understanding theories that give the graviton a mass. This thesis considers several aspects of these massive spin-2 effective field theories and related theories. These theories are first studied from the perspective of scattering amplitudes. The most general 2 → 2 scattering amplitude is constructed for theories containing a single massive graviton or vector. These amplitudes are then used to find the highest strong coupling scales in such theories, assuming a particular scaling of fields and momenta. Generalisations to include additional fields and self-interactions for massive higher-spin fields are also discussed. Constraints that arise from the existence of an ultraviolet completion are then studied. It is shown using dispersion relation arguments that the pseudo-linear massive spin-2 theory cannot admit an analytic, Lorentz-invariant, and unitary ultraviolet completion, but that such completions are not ruled out for massive vector theories. The behaviour of massive spin-2 theories under dimensional reduction is also explored. Stability conditions and the lower-dimensional spectrum are derived for the Kaluza-Klein dimensional reduction of a partially massless graviton and a massive graviton on an Einstein product manifold. Additionally, the nonlinear dimensional reduction of the zero modes in dRGT massive gravity is shown to produce a mass-varying massive gravity theory. Lastly, attempts to construct a version of unimodular gravity containing a massive graviton are discussed. A candidate theory is proposed and is shown to have pathologies. Dimensional reduction is then used to generate massive spin-2 theories with noncanonical kinetic terms and auxiliary fields. These theories are shown to be equivalent to the Fierz-Pauli theory, which provides further evidence for the uniqueness of the kinetic term used in dRGT massive gravity.

No description available.

Massive gravity is an extension of general relativity where the graviton, which mediates gravitational interactions, has a non-vanishing mass. The first steps towards formulating a theory of massive gravity were made by Fierz and Pauli in 1939, but it took another 70 years until a consistent theory of massive gravity was written down. This thesis investigates the phenomenological implications of this theory, when applied to cosmology. In particular, we look at cosmic expansion histories, structure formation, integrated Sachs-Wolfe effect and weak lensing, and put constraints on the allowed parameter range of the theory. This is done by using data from supernovae, the cosmic microwave background, baryonic acoustic oscillations, galaxy and quasar maps and galactic lensing. The theory is shown to yield both cosmic expansion histories, galactic lensing and an integrated Sachs-Wolfe effect consistent with observations. For the structure formation, however, we show that for certain parameters of the theory there exists a tension between consistency relations for the background and stability properties of the perturbations. We also show that a background expansion equivalent to that of general relativity does not necessarily mean that the perturbations have to evolve in the same way. / <p>At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 5: Manuscript. Paper 6: Manuscript.</p>

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第18793号 / 理博第4051号 / 新制||理||1583(附属図書館) / 31744 / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)教授 田中 貴浩, 教授 中村 卓史, 教授 高柳 匡 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

This thesis concerns a range of aspects of theoretical physics. It is composed of two parts. In the first part we motivate our line of research, and introduce and discuss the relevant concepts. In the second part, four research papers are collected. The first paper deals with a possible extension of general relativity, namely the recently discovered classically consistent bimetric theory. In this paper we study the behavior of perturbations of the metric(s) around cosmologically viable background solutions. In the second paper, we explore possibilities for particle physics with low-scale supersymmetry. In particular we consider the addition of supersymmetric higher-dimensional operators to the minimal supersymmetric standard model, and study collider phenomenology in this class of models. The third paper deals with a possible extension of the notion of Lie algebras within category theory. Considering Lie algebras as objects in additive symmetric ribbon categories we define the proper Killing form morphism and explore its role towards a structure theory of Lie algebras in this setting. Finally, the last paper is concerned with the computation of string amplitudes in four dimensional models with reduced supersymmetry. In particular, we develop general techniques to compute amplitudes involving gauge bosons and gravitons and explicitly compute the corresponding three- and four-point functions. On the one hand, these results can be used to extract important pieces of the effective actions that string theory dictates, on the other they can be used as a tool to compute the corresponding field theory amplitudes. / Over the last twenty years there have been spectacular observations and experimental achievements in fundamental physics. Nevertheless all the physical phenomena observed so far can still be explained in terms of two old models, namely the Standard Model of particle physics and the ΛCDM cosmological model. These models are based on profoundly different theories, quantum field theory and the general theory of relativity. There are many reasons to believe that the SM and the ΛCDM are effective models, that is they are valid at the energy scales probed so far but need to be extended and generalized to account of phenomena at higher energies. There are several proposals to extend these models and one promising theory that unifies all the fundamental interactions of nature: string theory. With the research documented in this thesis we contribute with four tiny drops to the filling of the fundamental physics research pot. When the pot will be saturated, the next fundamental discovery will take place.

Submitted by Douglas Benndorf Rodrigues null (dbenndorf@yahoo.com.br) on 2017-01-17T06:06:36Z No. of bitstreams: 1 HamiltVincSpin2_V7.pdf: 644680 bytes, checksum: 7826f04e2072b12f1597892b97b67791 (MD5) / Approved for entry into archive by LUIZA DE MENEZES ROMANETTO (luizamenezes@reitoria.unesp.br) on 2017-01-20T13:54:02Z (GMT) No. of bitstreams: 1 rodrigues_db_me_guara.pdf: 644680 bytes, checksum: 7826f04e2072b12f1597892b97b67791 (MD5) / Made available in DSpace on 2017-01-20T13:54:02Z (GMT). No. of bitstreams: 1 rodrigues_db_me_guara.pdf: 644680 bytes, checksum: 7826f04e2072b12f1597892b97b67791 (MD5) Previous issue date: 2016-12-19 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / Neste trabalho abordamos de forma introdutória o tratamento de sistemas singulares, em especial as teorias de Maxwell, Proca e Fierz-Pauli, e obtemos resultados originais para a família de modelos de spin-2 massivos do tipo não-Fierz-Pauli. Tendo como ferramenta principal o método de Dirac para sistemas vinculados, escrevemos a densidade de hamiltoniana primária do modelo LnF P , obtemos seus vínculos primários, secundários, terciários e quartenários, assim como os multiplicadores de Lagrange. Calculamos também o número de graus de liberdade independentes e mostramos a positividade da hamiltoniana reduzida. / In this work, we approach in an introductory way the treatment of singular systems, especially the theories of Maxwell, Proca and Fierz-Pauli, and obtain original results for the non-Fierz-Pauli family of massive spin-2 models. Having as main tool the Dirac method for constrained systems, we write the primary Hamiltonian density of the LnF P model, obtain their primary, secondary, tertiary and quaternary constraints, as well as Lagrange multipliers. We calculate the number of independent degrees of freedom of the model and demonstrate the positivity of the reduced Hamiltonian.

No description available.

La première partie de cette thèse traite des théories de gravité massive. L'étude de ces théories a connu un regain d'intérêt depuis la découverte de l'accélération de l'expansion de l'univers, car elles pourraient expliquer cette dernière sans avoir à recourir à une constante cosmologique. La découverte, en 2010 d'une théorie cohérente de gravité massive, dite dRGT, a ouvert un vaste et prometteur champ d'investigation. Dans cette thèse nous déterminons, dans une formulation métrique et covariante, la linéarisation autour d'espace-temps arbitraires de ces théories, et de leur extension bimétrique. Ce travail nous permet ensuite de compter par une méthode lagrangienne le nombre de degrés de liberté qui se propagent. La seconde partie de cette thèse s'inscrit dans le cadre des ondes gravitationnelles en relativité générale et porte plus précisément sur la dynamique de systèmes binaires d'objets compacts. Ce travail est important dans la perspective de leur détection par les détecteurs interférométriques d'ondes gravitationnelles terrestres et spatial. Nous étudions le problème de la dynamique de systèmes binaires d¿objets compacts en relativité générale, à l¿aide de la méthode d'approximation dites des développements post-newtoniens (PN). Nous dérivons les équations du mouvement à l'ordre $4$PN en coordonnées harmoniques. Nous utilisons une méthode basée sur une action de Fokker adaptée au formalisme post-newtonien, en dérivant notamment les effets de sillage d'onde qui apparaissent à $4$PN. / The first part of this thesis deals with massive gravity theories. There has been a renewal of interest in these theories since the discovery of the acceleration of the expansion of the universe, because they could explain it without having to resort to a cosmological constant. The discovery in 2010 of a coherent theory of massive gravity, named dRGT, has opened a vast and promising field of investigation. In this thesis we determine, in a metric and covariant formulation, the linearization around arbitrary backgrounds of these theories and their bimetric extension. This result then allows us to count with a Lagrangian method the number of degrees of freedom that are propagating. The second part of this thesis concerns gravitational waves in general relativity and especially the dynamics of coalescing compact binary systems. This work is important in view of their detection by interferometric detectors, both terrestrial and spacial. We study the dynamics of compact binary systems in general relativity, using the approximation method based on post-Newtonian developments (PN). We derive the equations of motion to $4$ PN order in harmonic coordinates. We use a method based on a Fokker action adapted to the post-Newtonian formalism, in particular deriving the tail effects appearing at $4$PN.