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.

Dans cette thèse nous étudions le problème de Cauchy en relativité générale. Motivés par la conjecture de censure cosmique faible formulée par Penrose, nous analysons le problème aux données initiales pour les équations d'Einstein dans le vide en faible régularité. Nous démontrons les deux résultats suivants. o Premièrement, nous nous intéressons aux équations de contrainte pour les données initiales et mettons en place une procédure de prolongement. Plus précisément, étant donné des données initiales pour les équations d'Einstein sur la boule unité dans R3, nous les prolongeons de manière continue en des données globales, asymptotiquement plates sur R3. Les équations de contrainte forment un système couplé d'équations non-lineaires sous-determinées géométriques. La preuve de notre procédure de prolongement repose sur un schéma iteratif où nous séparons ce système en deux problèmes de prolongement decouplés et solubles. Enfin, le résultat de prolongement pour les équations de contrainte est obtenu par un argument de point fixe. o Deuxièment, nous prouvons une version localisée du théorème de courbure L2 de Klainerman-Rodnianski-Szeftel. Nous montrons que, étant données des données initiales pour les équations d'Einstein sur une variété compacte avec bord, le temps d'existence de la solution des équations d'Einstein dans le domaine de dépendance de ces données initiales ne dépend que de normes de basse régularité des données initiales. En particulier, notre résultat est un critère localisé de continuité pour les équations d'Einstein. Notre preuve utilise un argument de localisation où, tout d'abord, nous généralisons la théorie de Cheeger-Gromov de convergence pour les variétés Riemanniennes à notre cas de régularité faible, et ensuite nous appliquons la procédure de prolongement pour les équations de contrainte mentionnée ci-dessus avec un argument de changement d’échelle. / In this thesis we study the Cauchy problem of general relativity. Motivated by the weak cosmic censorship conjecture formulated by Penrose, we analyse the initial value problem for the Einstein vacuum equations in low regularity. We prove the following two results. First, we consider the constraint equations of the initial data and demonstrate an extension procedure. More precisely, given small initial data for the Einstein equations on the unit ball in R3, we continuosly extend it to global, asymptotically flat initial data on R3. The constraint equations for the Einstein vacuum equations are a coupled system of non-linear under-determined geometric elliptic equations. The proof of our extension procedure is based on an iterative scheme where we split this system into two decoupled, solvable extension problems. The extension result for the constraint equations follows then by a fix point argument. Second, we prove a localised version of the bounded L2-curvature theorem by Klainerman-Rodnianski-Szeftel. We show that given low regularity initial data to the Einstein equations on a compact manifold with boundary, the time of existence of the solution to the Einstein equations in the domain of dependence of the initial data depends only on low regularity geometric data. In particular, this result is a localised continuation criterion for the Einstein vacuum equations. Our proof uses a localisation argument where we first generalise the known Cheeger-Gromov convergence theory for Riemannian manifolds to our low regularity setting, and then apply the above extension procedure for the constraint equations with a scaling argument.

Le but à long terme de mon travail de recherche est de trouver une alternative viable à la méthode conforme, qui nous permettrait de mieux comprendre la structure géométrique de l'espace des solutions des équations de contrainte. L'avantage du modèle de Maxwell (the drift model) par rapport aux modèles plus classiques est la présence des paramètres supplémentaires. Le prix à payer, par contre, sera que la complexité analytique du système correspondant. Ma thèse a été structuré en deux parties : a. Existence sous la condition de petitesse des données initiales. Nous avons montré que le système de Maxwell est raisonnable dans le sens où nous pouvons le résoudre, malgré sa forte nonliniarité, sous des conditions de petitesse sur ses coefficients, en dimension 3, 4 et 5. Par conséquent, l'ensemble des solutions est non-vide. b. Stabilité Nous montrons la stabilité des solutions du système: ce résultat est obtenu en dimension 3,4 et 5, dans le cas où la métrique est conformément plate, et le drift et petit / The long-term goal of my work is to find a viable alternative to the conformal method, which would allow us to better understand the geometry of the space of solutions of the constraint equations. The advantage of Maxwell's model (the drift model) is the presence of additional parameters. Its downside, however, is that it proves to be much more difficult from an analytic standpoint. My thesis is structued in two parts: a. Existence under suitable smallness conditions. We show that Maxwell's system is sufficiently reasonable: it can be solved even given the presence of focusing non linearities. We prove this under smallness conditions of its coefficients, and in dimensions 3,4 and 5. An immediate consequence is that the set of solutions is non-empty. b. Stability. We verify that the solutions of the system are stable: this result holds in dimensions 3,4 and 5, when the metric is conformally flat and the drift is small

The paper is located on the border between physics, mathematics and philosophy (ontology). The latter is required to embed the dualistic by nature mathematics into a monistic metatheory. It is shown, that a consequent philosophical monism and an approach which starts from the origin of the universe imposes significant constraints on a physical Theory-of-Everything. This may be helpful for finding such a theory. A philosophical system that is monistic and at the same time structured clear enough to be compatible with mathematical thinking is the Hegelian dialectic logic. With the aid of this logic the necessary existence of a causal chain embedded in the general, unconditional and timeless being is proved constructively. In the causal chain our entire reality is coded. It is termed by Hegel as determinate being in contrast to being. The chain has a beginning, representing the birth of the universe (big bang) and the beginning of time. It is isomorphic to the natural numbers. The half-ring structure of the natural numbers induces a secondary causal network. Thus the ontological approach results in a special version of the theory or causal sets. The causal network is topologically homeo-morphic to an infinite dimensional Minkowski cone. Each prime number corresponds to a dimension. Hypothetical small 'bumps” of 4D spacetime (Brane) in the direction of the extra dimensions of the Minkowski manifold mean topological defects, which can be interpreted as curvature of spacetime. This means a bridge to the general theory of relativity. On the other hand, the bumps may be interpreted as objects with which one can handle similar to the strings in string theory. / Die Arbeit bewegt sich im Grenzgebiet zwischen Physik, Mathematik und Philosophie (Ontologie). Letztere wird benötigt, um die vom Wesen her dualistische Mathematik in eine monistische Metatheorie einzubetten. Es wird gezeigt, dass ein konsequenter philosophischer Monismus und ein Denken vom Ursprung des Universums her einer physikalischen Theorie-von-Allem erhebliche Randbedingungen auferlegen. Für das Auffinden einer solchen Theorie kann das hilfreich sein. Ein philosophisches System, dass monistisch ist und zugleich klar genug strukturiert um mit der mathematischen Denkweise kompatibel zu sein ist die Hegelsche dialektische Logik. Unter Zuhilfenahme dieser Logik wird die notwendige Existenz einer in das allgemeine, unbedingte und zeitlose Sein eingebetteten, aber vom Chaos dieses Seins unbeeinflussten kausalen Kette konstruktiv bewiesen. In dieser kausalen Kette ist unsere gesamte Realität codiert, von Hegel als Dasein im Gegensatz zum Sein bezeichnet. Die Kette hat einen Anfang, der den Anfang des Universums und den Anfang der Zeit darstellt. Sie ist isomorph zu den natürlichen Zahlen. Deren Halbring-Struktur induziert ein sekundäres kausales Netzwerk. Somit ist das Ergebnis der ontologischen Herangehensweise eine spezielle Version der Theorie der kausalen Mengen. Das Netzwerk ist topologisch homöomorph ist zu einem unendlich dimensionalen Minkowski-Kegel. Jeder Primzahl entspricht eine Dimension. Hypothetische kleine „Ausbeulungen“ oder „Bumps“ der 4D-Raumzeit (Brane) in Richtung der Extradimensionen der Minkowski-Mannigfaltigkeit bedeuten topologische Baufehler, die sich als Krümmung der Raumzeit interpretieren lassen und eine Brücke zur allgemeinen Relativi-tätstheorie darstellen. Auf der anderen Seite lassen sich die Ausbeulungen der Brane als Objekte deuten, mit denen man ähnlich umgehen kann wie mit den Strings der Stringtheorie.

The main result of the thesis is the derivation of quantum phenomenological gravi- tational dynamics from the thermodynamics of local causal diamonds. By taking into account logarithmic corrections to entropy implied by quantum gravity effects, we derive new gravitational equations of motion which incorporate quantum corrections. The re- sulting theory appears to be a direct generalisation of the classical unimodular gravity instead of the general relativity. Upon obtaining the equations, we discuss their prop- erties and possible implications. As by-products, we also present a novel derivation of the Einstein equations from the thermodynamics of causal diamonds and a derivation of the logarithmic corrections to black hole entropy from the existence of minimal re- solvable area. Apart from the new results, we also provide an extensive review of the thermodynamics of local causal horizons. 1

Black holes are one of the most interesting objects in the universe, and studying these objects should give exciting results. This research will investigate the General Theory of Relativity, explaining the essence of the theory needed for deriving solutions for a Schwarzschild black hole. This knowledge leads to deriving the equations of motion of a bosonic scalar field around a Schwarzschild black hole. Computing the dynamical evolution of that scalar field, and taking the limit far away from the black hole, gives an approximation derivation of the  Schrödinger equation. This study opens many doors to future research about black holes and scalar fields. / Svarta hål är ett av de mest intressanta objekten i universum, och därför, att studera dessa föremål bör ge spännande resultat.I detta arbete kommer den allmänna relativitetsteorin  att studeras och förklaras med allt som behövs för att härledalösningar för en Schwarzschild svart hål. Denna kunskap leder till att härleda rörelseekvationerna för ett bosoniskt skalärfält runt ett Schwarzschild svart hål.Genom att beräkna den dynamiska utvecklingen av det skalära fältet och ta gränsen långt bort från svarta hålet,så kommer det at ge en approximativ härledning av Schrödinger ekvationen. Den här typen av studier öppnar många dörrar för framtida forskning om svarta hål och skalära fält.

Astrophysical observations of the cosmic microwave background point to inconsistencies in the standard model of cosmology, and a primordial accelerated expansion of the universe known as inflation has been suggested as a solution. Unfortunately, observational evidence of inflation is lacking, and there exists hundreds of models that populate the inflationary landscape. In this thesis, we explore three of these and see what constraints are set on them in order to account for observations. We find that two of the models have regimes of trans-planckian nature, while the third leads to a non-invertible equation. / Astronomiska observationer av den kosmiska bakgrundsstrålningen tyder på bristfälligheter i standardkosmologin, vilket har lett till förslaget om en accelererande expansion i de tidigaste skeden av universum känd som inflation. I avsaknaden av observationella bevis finns det numera hundratals inflationsmodeller, och i detta arbete kommer vi att rikta fokuset mot tre av dessa avvilka två visar sig överstiga transplanckianska värden medan den sista leder till en ekvation som inte är inverterbar.

We extend previous work (2020Class. Quantum Grav. 37 075001)to the case of Maxwell’s equations with a source. Our work shows how to construct a vector potential for the Maxwell field on the Kerr–Newman background in a radiation gauge. The vector potential has a ‘reconstructed’ term obtained from a Hertz potential solving Teukolsky’s equation with a source, and a ‘correction’ term which is obtainable by a simple integration along outgoing principal null rays. The singularity structure of our vector potential is discussed in the case of a point particle source

The aim of this work is to derive mathematical descriptions of gravitation. Postulating gravitation as a force field, Newton's law of gravitation is heuristically derived by considering linear differential operators invariant under euclidean isometries and by finding the fundamental solution to Helmholtz equation in three dimensions. Thereafter, the theory of differential geometry is introduced, providing a framework for the subsequent review of gravitation as curvature. Lastly, in the light of Einstein's postulates and equivalence principle, Lovelock's proof of uniqueness of Einstein's field equations is presented.

<p dir="ltr">Neutron star mergers generate powerful gravitational waves and various types of electromagnetic signals, including gamma-ray bursts (GRB), kilonovae, and their afterglows. Observing and modeling these signals help us understand the physical processes of the merger events. Radiation from mergers can also serve as probes to study nuclear physics and cosmology. In this report, I focus on two types of signals: the GRB afterglow and the kilonova. GRB afterglows are non-thermal radiation produced by the interaction of relativistic jets and circumburst material, where the jets are launched perpendicular to the merger plane. Kilonovae are the thermal radiation emitted from the hot materials ejected during the merger. Besides the modeling of these objects, I also investigate their application in multimessenger astrophysics, especially the constraint on the expansion rate of the Universe. </p><p dir="ltr">First, I developed a GRB afterglow model to account for the off-axis observation of a structured jet. Using a jet structure derived from a three-dimensional general relativistic magnetohydrodynamic simulation, we performed a joint analysis of the multimessenger data of the neutron star merger event GW170817, including the gravitational wave data and GRB afterglow data in the radio band. We have tightly constrained the observing angle of GW170817 and broken the degeneracy between the inclination angle and luminosity distance measured in gravitational waves. With a better constrained distance, we improved the standard siren measurement of the Hubble constant to $H_0 = 69.5\pm 4\ \mathrm{km\ s^{-1}\ Mpc^{-1}}$. The error bar has been reduced by a factor of 2. This work demonstrates that the modeling of off-axis GRB afterglow can significantly improve the standard siren method, provided that we have a reliable jet structure.</p><p dir="ltr">Second, I upgrade the GRB afterglow model in the first work, extending it to the late time where lateral spreading of the GRB jet becomes important. In this model, the ultra-relativistic blastwave is approximated by an infinitely thin two-dimensional surface. With this approximation, the hydrodynamic equations can be analytically integrated over the radius. Further assuming axial symmetry, the three-dimensional hydrodynamic simulation can be reduced to one dimension, which significantly increases the computational efficiency. We have compared our method to full numerical simulations and existing GRB afterglow modeling tools. The comparison shows good agreement and verifies our approach. Compared to these tools, our model has better flexibility and is applicable in a broader context. This method has been developed into a numerical code, \texttt{jetsimpy}, which we have provided to the community. It will serve as a powerful tool in the era of multimessenger astrophysics.</p><p dir="ltr">Finally, I investigate the possibility of long-lived massive neutron stars as neutron star merger remnants. A long-lived massive neutron star can inject a significant amount of energy into the merger ejecta, boosting the luminosity of kilonova by several orders of magnitude. However, this type of event has not yet been observed in optical sky surveys. We developed a boosted kilonova model with a detailed calculation of the photoionization process to better describe the efficiency of energy injection from spin down power to the ejecta. Our study found that boosted kilonovae, if commonly occurring, they should have already been observed given the accumulated time in sky surveys. As a result, the absence of detection implies that long-lived massive neutron stars as neutron star merger remnants are likely to be rare in the Universe.</p>