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Made available in DSpace on 2016-12-23T14:20:02Z (GMT). No. of bitstreams: 1 Junior Diniz Toniato.pdf: 412954 bytes, checksum: 2559260e7dcddc93c1ce6baff90a288d (MD5) Previous issue date: 2010-07-29 / There isn t experimental evidences that can validate the results of black holes termodynamics. This because the radiation emitted by the black hole, predicted by theory, it is almost impossible to be detected due to its low value of magnitude. In the search for clues that could validate the existence of this radiation, the study of analog models to those objetcs has grown considerably in recent decades. They allow the idealization of experiments in labs that would be extremely complicate to be done directly with the gravitational systems. A fluid in moviment can act on the sound the same way that curved space-time can influence on light trajectory in the general relativity. So, one can describe the propagation these sound waves through an effective metric, under wich they will follow null geodesics. This thesis makes a review of these studies focusing in an analogy to Schwarzschild black hole using an acoustic system, showing its advantages and limitations when applied in the study of Hawking s theory / Ainda não há uma comprovação experimental que possa validar os resultados obtidos da termodinâmica de buracos negros. Isso porque a radiação emitida pelo buraco negro, prevista pela teoria, é praticamente impossível de ser detectada devido ao baixo valor de sua ordem de grandeza. Na busca por indícios que possam validar a existência dessa radiação, o estudo de modelos análogos a esses objetos tem crescido consideravelmente nas últimas décadas. Eles permitem a idealização de experimentos em laboratórios que seriam impossíveis de serem realizados diretamente nos sistemas gravitacionais. Um fluido em movimento pode agir sobre o som da mesma forma que os espaçotempos curvos podem influenciar na trajetória da luz na relatividade geral. Com isso, pode-se descrever a propagação dessas ondas sonoras através de uma métrica efetiva, sob a qual elas seguirão geodésicas nulas. Esta dissertação faz uma revisão destes estudos concentrando-se em uma analogia acústica para um buraco negro de Schwarzschild, demonstrando suas vantagens e limitações quando aplicada para o estudo da teoria de Hawking

In this thesis we study exact general relativistic space-times generated by a black hole and an additional source of gravity, while restricting to two classes of static and axially symmetric solutions: the Majumdar-Papapetrou solution for a couple (in general, a multiple system) of extremally charged black holes and the "superposition" of a Schwarzschild black hole with the Bach-Weyl thin ring. We follow the effect of the additional source on the geometry of black-hole space-time on the behaviour of important invariants, in particular of the simplest scalars obtained from the Riemann and possibly also Ricci tensor. We have plotted the invariants both outside and inside the black hole; in the case of a Schwarzschild black hole with ring, we found, to this end, an extension of the metric below the horizon. It turns out that the external source may affect the geometry inside the black hole considerably, even in the vicinity of singularity, although the singularity itself remains point-like in both solutions studied here.

Made available in DSpace on 2015-04-22T22:07:28Z (GMT). No. of bitstreams: 1 RICARDO_HERCULANO.pdf: 868447 bytes, checksum: 0c36ef607bb3e267e05d3dc5c7242880 (MD5) Previous issue date: 2005-02-17 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior / In this work we studied the time evolution of the hole states of the valence sub-band of a heteroestructure quantum well type with effective width time periodically dependent. Although of the experimental point of view this work not to be possible, we can imagine a mechanism through which the active region of confinement is modified of periodic form. We study of detailed form the effect of the coupling (kk 6= 0), between bands HH and LH on the wave functions envelope, we analyze the probabilities of transistion in subbandas HH1 and LH1, effect this known as "mixing" of the valence subbands. To develop this study we made use of the time evolution operator applied the wave functions envelope that had been gotten by mass effective equation for the Luttinger Hamiltonian. We compare the results gotten with the results of another work, where the system evolves with constant speed, thus analyzing the differences in the evolutions. Unhappily we do not find in literature references regarding evolutions with periodic speed, what it disabled possible comparisons. / Neste trabalho estudamos a evolução temporal dos estados de buracos da banda de valência de uma heteroestrutura tipo poço quântico com largura efetiva dependente periodicamente do tempo. Apesar de, do ponto de vista experimental, este trabalho não ser possível, podemos imaginar um mecanismo através do qual a região ativa de confinamento seja alterada de forma periódica. Estudamos de forma detalhada os efeitos do acoplamento (fórmula), entre as bandas HH e LH sobre as funções de onda envelope, analisamos as probabilidades de trasição nas subbandas HH1 e LH1, efeito esse conhecido como "mixing" entre sub-bandas . Para desenvolvermos esse estudo fizemos uso do operador evolução temporal aplicado às funções de onda envelope que foram obtidas via equação de massa efetiva para o Hamiltoniano de Luttinger. Comparamos os resultados obtidos com os resultados de outros trabalhos, onde o sistema evolui com velocidade constante, analisando assim as diferenças nas evoluções. Infelizmente não encontramos na literatura referências a respeito de evoluções com velocidade periódica, o que impossibilitou possíveis comparações.

Made available in DSpace on 2015-04-22T22:07:29Z (GMT). No. of bitstreams: 1 SALOME_ FONTAO_CUNHA.pdf: 1002004 bytes, checksum: d7451d75aca7e8b7ef22bdbdd99db48c (MD5) Previous issue date: 2005-07-29 / Conselho Nacional de Desenvolvimento Científico e Tecnológico / Estudamos o transporte de buracos em dupla barreira ressonante submetida a stress uniaxial, usando a técnica da matriz de espalhamento na aproximação de massa efetiva do modelo de Luttinger-Kohn-Pikus. A transmissividade é calculada para k = 0 e k ≠ 0 para o sistema GaAs /AlAs para os esforços de compressão (T < 0) e tração (T > 0). Para k = 0, os buracos leves e pesados são desacoplados e observa-se um deslocamento rígido nas curvas de transmissividades e inversão do estado fundamental, HH1 LH1 para o esforço de tração. No caso k ≠ 0, além da mistura das bandas que aumenta a probabilidade de transmissão, o stress muda o caráter das partícula HH LH, a separação relativa entre os estados HH e LH no poço quântico, e indiretamente, influência na mistura dos estados de valência, aumentando ou diminuindo as transmissividades dos buracos dependendo do tipo de esforço aplicado.

General relativity, one of the pillars of our understanding of the universe, has been a remarkably successful theory. It has stood the test of time for more than 100 years and has passed all experimental tests so far. Most recently, the LIGO collaboration made the first-ever direct detection of gravitational waves, confirming a long-standing prediction of general relativity. Despite this, several fundamental mathematical questions remain unanswered, many of which relate to the global existence and the stability of solutions to Einstein's equations. This thesis presents our efforts to use numerical relativity to investigate some of these questions. We present a complete picture of the end points of black ring instabilities in five dimensions. Fat rings collapse to Myers-Perry black holes. For intermediate rings, we discover a previously unknown instability that stretches the ring without changing its thickness and causes it to collapse to a Myers-Perry black hole. Most importantly, however, we find that for very thin rings, the Gregory-Laflamme instability dominates and causes the ring to break. This provides the first concrete evidence that in higher dimensions, the weak cosmic censorship conjecture may be violated even in asymptotically flat spacetimes. For Myers-Perry black holes, we investigate instabilities in five and six dimensions. In six dimensions, we demonstrate that both axisymmetric and non-axisymmetric instabilities can cause the black hole to pinch off, and we study the approach to the naked singularity in detail. Another question that has attracted intense interest recently is the instability of anti-de Sitter space. In this thesis, we explore how breaking spherical symmetry in gravitational collapse in anti-de Sitter space affects black hole formation. These findings were made possible by our new open source general relativity code, GRChombo, whose adaptive mesh capabilities allow accurate simulations of phenomena in which new length scales are produced dynamically. In this thesis, we describe GRChombo in detail, and analyse its performance on the latest supercomputers. Furthermore, we outline numerical advances that were necessary for simulating higher dimensional black holes stably and efficiently.

Les cycles d’hysteresis des binaires X lors de leurs sursauts restent inexpliqués a ce jour. Dans ce travail, nous avons développé les idées du paradigme propose par Ferreira et al. (2006), ou la matière dans le disque accrète de deux manières différentes. Dans le mode standard (SAD, Shakura et Sunyaev 1973), le couple turbulent transporte le moment cinétique radialement vers l’extérieur du disque. Dans le mode éjectant (JED, Ferreira et Pelletier 1995), le disque magnetise produit des jets qui emporte la matière, l’énergie et le moment angulaire verticalement. Dans ce cadre, la transition entre les deux modes est liée a la distribution de champ magnétique dans le disque, une inconnue. Pendant cette thèse, j’ai développé un code capable de résoudre a chaque rayon dans un disque l’équilibre thermique a deux températures pour de multiples jeu de paramètres. Ce code utilise Belm (Belmont et al. 2008 ; Belmont 2009) pour traiter le refroidissement radiatif et créer les spectres de manière auto-cohérente. Les processus de chauffage sont analytiques, ainsi que les processus d’advection, qui sont calcules de l’interieur vers l’exterieur.Grace a ce code, nous avons pu montrer que des solutions de JED reproduisaient très bien les états hard jusqu’à 0.5 luminosités d’Eddington (Marcel et al. 2018a). Il a aussi été démontré que le JED subit un cycle d’hysteresis. En revanche, la luminosité de ce cycle est bien trop faible et la présence inévitable de jets dans la configuration nous pousse a l’utilisation d’un SAD pour la reproduction d’états soft.Fort de ces résultats, j’ai adapte le code a la résolution de configuration de disque hybride, compose d’un JED interne et d’un SAD externe, séparé en un rayon de transition rJ. En jouant sur ce paramètre rJ et sur le taux d’accrétion mdot, nous avons pu montrer que les observations X de cycles typiques pouvaient être pavée. Après des calculs similaires a Heinz et Sunyaev (2003), nous pouvons estimer quel est le flux radio associe a chaque jeu de paramètres. Cela nous a permis de montrer 2 choses. (1) tous les flux radios sont reproductibles a l’aide d’un seul facteur de normalisation commun. (2) le flux radio et la forme du spectre en rayons X sont cohérents : les jeux de paramètres qui reproduisent le mieux chaque forme spectral sont associes aux bon flux radios. Afin d’illustrer ce résultat, 5 états canoniques de l’évolution de GX 339-4 ont ete reproduits : forme spectrale en X et flux radios (Marcel et al. 2018b). Pour finir, en utilisant une simple procédure d’ajustement sur la forme spectrale en X, le cycle de 2010-2011 de GX 339-4 a pu être reproduit. De manière bluffante, les évolutions de rJ et mdot semblent être en accord avec les prédictions théoriques (Esin et al. 1997). De plus, les estimations de flux radio étant cohérentes avec les observations, nous avons décidé de les ajouter directement dans la procédure d’ajustement. L’ajout de cette composante a permis une excellente reproduction simultanée de la radio et des spectres X de manière. C’est, a notre connaissance, la première fois que les phénomènes d’accrétion et d’éjection sont utilisés simultanément. Ces résultats, ainsi que les discussions et implications seront bientôt soumis. / The hysteresis behavior of X-ray binaries during their outbursts remains a mystery. In this work, we developed the paradigm proposed in Ferreira et al. (2006) where the disk material accretes in two possible, mutually exclusive, ways. In the standard accretion disk (SAD, Shakura et Sunyaev 1973) mode, the dominant local torque is due to MHD turbulence that transports radially the disk angular momentum. In the jet-emitting disk (JED, Ferreira et Pelletier 1995) mode, magnetically-driven jets carry away mass, energy and all the angular momentum from the disk. Within our framework, the transition from one mode to another is related to the magnetic field distribution, an unknown yet.In this thesis, I have developped a two-temperature plasma code able to compute the thermal balance at each radius for a large ensemble of disk parameters, as well as the self- consistent global emitted spectrum. The radiative cooling term and related spectrum (comptonized bremsstrahlung and synchrotron emission) are obtained using the Belm code (Belmont et al. 2008 ; Belmont 2009). Heating processes are analytical and due only to accretion, while advection is properly taken into account, carrying outside-in the memory of the outer thermal states.Using this code, we have shown that a JED extending along the entire disk nicely repro- duces hard states up to 0.5 Eddington luminosities (Marcel et al. 2018a). It was also shown that JEDs produce a natural hysteresis cycle. However, the global luminosity of the cycle is insufficient and the inevitable presence of jets in JEDs advocates for an inner SAD configuration in soft states.Based on these results, the code was enhanced to solve hybrid configurations with an internal JED and an external SAD, separated by a given transition radius rJ. Playing on both rJ and the accretion rate mdot, we have shown that X-ray observations of typical cycles can be completely covered. Using a simple synchrotron model similar to that of Heinz et Sunyaev (2003), the radio flux produced by the jets can be estimated, showing two important features. First, all radio observations can be covered by our model. Second, the radio flux and X- ray spectral coverages are consistents : parameter sets that reproduce best each spectral state also account for a consistent associated radio flux. For illustration, 5 canonical states from GX 339-4 have been reproduced in X-ray spectral shape and associated radio fluxes (Marcel et al. 2018b).Finaly, using a simple fitting procedure on X-ray spectral shape, the 2010-2011 cycle from GX 339-4 has been reproduced. Strikingly, the co-evolution of rJ and mdot seems to be in adequacy with initial theoretical expectations (Esin et al. 1997). Moreover, the estimated radio flux evolution being close to observations, we decided to use those within the fitting procedure. Adding radio fluxes constraints in the procedure allowed us to reproduce both the associated X-ray spectral shape and radio fluxes with excellent agreement. This is, to our knowledge, the first time that such an accretion-ejection cycle is reproduced. Those results, as well as discussions and implications will be soon submitted.

Esta tese é um estudo de estabilidade de modos quasinormais em um sistema que apresenta uma mudança de estabilidade ao variar continuamente os parâmetros físicos de um buraco negro. A mudança de estabilidade encontrada possui interpretações na correspondência AdS/CFT. A ferramenta principal utilizada neste trabalho para o cálculo de modos quasinormais foram métodos numéricos que podem ser utilizados em inúmeros trabalhos desta área de pesquisa, especialmente por não dependerem de suposições de simetria ou de comportamento conveniente do sistema físico. / This thesis is a study of stability of quasinormal modes in a system featuring a stability change if one continuously varies the physical parameters of a black hole. The stability change thus found has some possible interpretations in the AdS/CFT correspondence. The main tool used in this study for calculating quasinormal modes are numerical methods that can be used in numerous works in this area of research, especially because they do not depend on assumptions of symmetry or any convenient behavior of the physical system.

Neste trabalho faremos uma investigação no campo das perturbações gravitacionais e propagação de ondas em geometrias de buracos negros com campos elétricos ou magnéticos. Usando uma geometria tipo Ernst-Melvin de um buraco negro massivo em um Universo com campo magnético no eixo z, calculamos os modos quasi-normais de propagação de um campo escalar, demonstrando que este se comporta como um campo escalar com massa 2|m|B em uma geometria de Schwarzschild, para pequenos valores do campo magnético B (correspondendo m ao número azimutal do esférico harmônico). Ainda com esta geometria, calculamos a contribuição de ondas escalares para a entropia do buraco negro em termos dos cut offs ultravioleta e infravermelho. Com uma solução do tipo Reissner-Nordström em 4 dimensões, investigamos as possíveis correspondências entre os modos quasinormais e as propriedades termodinâmicas deste buraco negro, atestando o resultado de que a conjectura Hod modificada por Maggiore é válida em tal solução. Também, com uma geometria de Reissner-Nordström-de Sitter D-dimensional, obtivemos os modos quasi-normais de vibração para dois potenciais diferentes, estabelecendo a ausência de modos instáveis para uma grande gama de parâmetros deste buraco negro. / In this work we make an incursion into the branch of gravitational perturbations and field propagation around known-geometries of black holes with electromagnetic fields. Using an Ernst-Melvin type of geometry in a massive black hole immersed on a magnetic Universe, we calculate the quasi-normal modes of the propagating field, showing the equivalence of this problem with that of a massive scalar field (for which the mass is 2|m|B, m being the azhimutal number, and B the magnetic field) propagating around a Schwarzschild geometry. We also compute the contribution of the scalar field to the entropy of the black hole in terms of the infrared and ultraviolet cut offs. Using a Reissner-Nordstr¨om-like solution in 4 dimensions, we investigate the possible correspondence between quasi-normal modes and the thermodynamical properties of this black hole, atesting the validity of the modified Hod conjecture as proposed by Maggiore. Finally, for a Reissner-Nordstr¨om-de Sitter D-dimensional solution, we obtain the quasi-normal modes for two diferent potentials, establishing the absence of unstable modes for a large range of values for the black hole parameters.

Ultraluminous X-ray (ULX) sources are non-nuclear extragalactic accreting compact objects whose X-ray luminosities exceed the Eddington limit for stellar mass black hole binaries (BHB). Their high luminosities suggest they are either intermediate mass black holes, that their emission is beamed, or that they are emitting at super-Eddington rates. We observed the ULX IC 342 X-1 simultaneously in X-ray and radio with Chandra and the VLA to investigate previously reported unresolved radio emission coincident with the ULX. The Chandra spectrum appears to be consistent with an accretion disc-dominated thermal state and suggests a mass of the black hole using the modeled inner disc temperature to be 157Mʘ ≤ M √ (cosi) ≤ 200 Mʘ. No significant radio emission was observed, consistent with the source being in a thermal disc-dominated state. Reanalysis of previous X-ray observations of the source shows that high energy curvature often interpreted as evidence for supercritical accretion cannot confidently be identified using the 2-10 keV energy band. Black hole systems such as BHBs, ULXs, and AGN represent the greatest test labs in the universe for the study of extreme gravity. Emission from the accretion disk and scattering from the surrounding corona allow study of the ultra-strong gravity and magnetic fields very near the central BH engine. However, many of these effects are imprinted as polarization of the emission and are invisible to spectral and timing studies alone. The outflows from AGN are also thought to play a key role in galaxy shaping and cluster formation. High efficiency and spectral resolution are required to measure ionization-velocities and density parameters from these sources to constrain the outflow structure. Beamline studies and theoretical modeling were carried out to characterize the throughput and spectral resolving power of off-plane gratings for use in future x-ray observatories which will make these measurements. Additionally, synchrotron measurements were carried out to test theoretical predictions of strong polarization response for off-plane diffraction gratings. The empirical results of this study are the first to demonstrate a lack of polarization sensitivity for grazing-incidence off-plane gratings and support more complex modeling results than used previously.