O objetivo principal deste trabalho é estudar a interação dos buracos negros primordiais com as principais espécies físicas exóticas de matéria e energia que foram teorizadas para explicar as observações cosmológicas da última década. A interação com diferentes formas de energia escura a partir de campos escalares, como a energia phantom, e modelos de quartessência, como o gás de Chaplygin, associada a modelos já existentes de interação com espécies físicas mais bem conhecidas, fornece resultados importantes e sugere comportamentos inesperados na trajetória dos buracos negros primordiais desde a sua formação até os dias de hoje. Nossa análise abrange os aspectos dinâmicos e termodinâmicos da acreção e evaporação de buracos negros, explorando os limites de validade da teoria e estudando o comportamento sob as condições extremas que resultam desses novos modelos de matéria e energia. Finalmente, o estudo prossegue na direção de um modelo de evolução a partir diretamente das equações de campo, em um espaço-tempo totalmente dinâmico em que buscamos paralelos com as descrições provenientes das hipóteses simplificadoras sobre que nos baseamos durante os estágios anteriores. Os resultados permitem fazermos uma descrição unificada da evolução dos buracos negros, em que as relações entre todas as componentes são transparentes e suas contribuições individuais são facilmente identificadas. Associando-os à descrição termodinâmica, é possível traçar um quadro completo e abrangente do problema, capaz de acomodar novos modelos e prover uma compreensão profunda da interação dos buracos negros com o meio cosmológico. / We study the interaction between primordial black holes and the exotic dark matter and dark energy components which have been modeled to explain cosmological observations within the last decade. The interaction with different forms of scalar field dark energy, such as phantom energy, and quartessence models as the Chaplygin gas, together with the well-known interaction with the ordinary forms of matter and energy, provides important results and suggests unexpected behaviors on primordial black holes since their formation until the present time. Our analysis encompasses dynamical and thermodynamical aspects of black hole accretion and evaporation exploring the theory validity ranges and studying its behavior under the extreme conditions which arise from these new dark fluid models. Finally, our study progresses towards an evolution model based solely on the field equations, within a fully dynamical space-time in which we seek parallel descriptions with previous models, which use simplifying hypotheses. Our results provide a unified description of black hole evolution, in which the role of all components and their relation to each other are clear and easily identifiable. Along with the thermodynamical description, it is possible to make a comprehensive picture of the problem, capable of accommodating new models and furnish a deep understanding of black hole interaction with the cosmological environment.

We study the evolution of binary black hole initial data schemes as alternatives to the standard puncture construction. These alternatives are based on post-Newtonian expansions that contain realistic gravitational waves. The first scheme is based on a second order post-Newtonian expansion in Arnowitt, Deser, and Misner transverse-traceless (ADMTT) gauge that has been re-summed to approach standard puncture data at the black holes. The other schemes are based on asymptotic matching of the 4-metrics of two tidally perturbed Schwarzschild solutions to post-Newtonian expansions at different orders. The alternatives are encouraging and lead to quasi-circular orbits and show gravitational radiation from the onset, as well as a reduction of spurious radiation. Deficiencies compared to punctures include more eccentricity during inspiral and larger constraint violations, since the alternative data sets only approximate solutions of Einstein's equations. / by George C. Reifenberger. / Thesis (Ph.D.)--Florida Atlantic University, 2013. / Includes bibliography. / Mode of access: World Wide Web. / System requirements: Adobe Reader.

Neste trabalho, construímos novas soluções com simetria esférica ou axial para as equações do campo gravitacional induzido num cenário brana do tipo Randall-Sundrum, onde uma 3-brana com constante cosmológica está imersa num espaço-tempo 5-dimensional conhecido como bulk. Para o caso esfericamente simétrico, com constante cosmológica negativa, obtivemos uma família de soluções numa brana assintoticamente anti-de Sitter, sendo que cada membro desta é diferenciado de outro por uma constante integração C, que fixada proveu-nos soluções de buracos negros ou buracos de minhocas. Com a mesma simetria, geometrias que descrevem buracos de minhoca foram encontradas numa brana assintoticamente de Sitter. Para o caso axialmente simétrico, métricas assintoticamente anti-de Sitter e de Sitter foram construídas no contexto citado. Propriedades óticas, como a rotação do vetor de polarização, foram estudadas, mostrando-nos algumas diferenças entre os mundos brana, tratados como uma teoria de gravitação modificada, e a relatividade geral. / In this work we have constructed new solutions, with axial or spherical symmetry, to the induced gravitational field equations within a Randall-Sundrum type brane world scenario, where a 3-brane with cosmological constant is embedded in a 5-dimensional space-time called bulk. For the spherical case with negative cosmological constant, we have found a family of solutions in an anti-de Sitter brane, where each member of the family is different from another when C is fixed. With a fixed C we have black holes or wormholes. In this same case, with spherical symmetry, we have obtained wormhole solutions in a de Sitter brane. In the same context, for the axially symmetric case, metrics asymptotically anti-de Sitter and de Sitter were built. Optics features, like rotation of polarization vector, have been studied. These features showed some differences between brane worlds, a theory of modified gravity, and the General Relativity.

Nesta tese, nós estabelecemos algumas correspondências entre a dinâmica de campos escalares clássicos em certos espaço-tempos de fundo e duais algébricos apropriados. Os cenários estudados incluem soluções tipo buraco negro com constante cosmológica não nula e os espaçostempos conhecidos como geometrias quase-extremas. Com base em várias propostas na literatura, associamos certos elementos próprios da dinâmica escalar a uma representação apropriada de uma álgebra relacionada com a invariância das equações de movimento escalar sob transformações conformes. Em particular, nós associamos representações de peso maior de dimensão infinita da álgebra sl(2,R) com modos e frequências quase-normais de campo escalar em geometrias quase-extremas e geometrias assintóticamente Anti de Sitter. / In this thesis, we establish some correspondences between dynamics of classical scalar fields in certain background spacetimes and appropriate algebraic duals. The scenarios studied include black hole solutions with non-zero cosmological constant and the spacetimes known as near extremal geometries. Based on several proposals in the literature, we associate certain elements proper to scalar perturbative dynamics to an appropriated representation of an algebra related with the invariance of the scalar equations of motion under conformal transformations. In particular, we associate infinite dimensional highest weight representations of the algebra sl(2,R) to quasinormal modes and frequencies of scalar fields in near extremal geometries and asymptotically Anti de Sitter geometries.

O crescente uso de lajes sem vigas (lisa com ou sem capitel) como solução estrutural de edificações, justificado por questões econômicas e construtivas, têm destacado a importância do estudo desses elementos estruturais. Já as desvantagens desse sistema estrutural estão associadas às altas tensões geradas na região próxima dos pilares, originando o fenômeno de punção. As normas atuais especificam uma seção íntegra resistente para dimensionamento à punção, entretanto, devido principalmente à passagem de instalações hidráulicas e elétricas através dos pavimentos, é necessária a execução de furações, em alguns casos muito próximas ao contorno dos pilares, o que implica diretamente na redução dessa seção e da resistência das lajes. Portanto, são necessários modelos de cálculo específicos para isso. A NBR 6118 tem critérios para esse problema, mas são antigos e precisam ser modernizados. Assim, comparando os dados experimentais de algumas pesquisas com as cargas últimas estimadas para normas vigentes (fib MC2010:2013, EC2:2004, ACI-318:2014 e NBR 6118:2014), este trabalho teve como objetivo identificar limitações das normas estudadas e verificar a eventual possibilidade de melhorias. Com base nos resultados observados foi proposta uma alteração para a NBR 6118: 2014 no cálculo da punção para lajes lisas com furo(s) na região do pilar, de modo que seja considerado no dimensionamento o momento gerado pela excentricidade do perímetro crítico devido à presença de furo(s) na laje. / The increasing use of flat slabs (slabs without beams with or without drop panel) as a structural solution of buildings, justified by economic and constructive issues, has highlighted the importance of the study of these structural elements. The disadvantages of this structural system are associated with high stresses generated in the region near of the columns, causing the punching shear phenomenon. The current standards specify a resistant section for punching shear design, however, due mainly to the passage of hydraulic and electric installations through the floors, it is necessary to execute holes, in some cases very close to the boundaries of the columns, which reduces this section and the slab strength. Therefore, it is necessary to specify calculation models for that. The NBR 6118 has criteria for this problem, nonetheless it is old and needs to be modernized. Comparing experimental data from some researches, with the estimated ultimate loads for current standards (fib MC2010: 2013, EC2: 2004, ACI-318: 2014 and NBR 6118: 2014), this work had as objective to identify limitations of the standards studied and verify possible improvements. Based on the observed results, it was proposed a modification for NBR 6118: 2014 in the design of the punching shear of flat slabs with hole(s) near of the column, considering the moment caused by the eccentricity of the critical perimeter due to the presence of hole(s) in the slab.

Mak Ka Wai Charles. / Thesis submitted in: October 2001. / Thesis (M.Phil.)--Chinese University of Hong Kong, 2002. / Includes bibliographical references (leaves 89-91). / Text in English; abstracts in English and Chinese. / Mak Ka Wai Charles. / Chapter 1 --- Introduction --- p.1 / Chapter 1.1 --- Overview of the Mathematical Framework --- p.2 / Chapter 1.2 --- System of Interest --- p.7 / Chapter 1.2.1 --- Klein-Gordon equation --- p.7 / Chapter 1.2.2 --- QNM boundary conditions --- p.12 / Chapter 1.3 --- Outline of This Thesis --- p.14 / Chapter 2 --- Green's Function --- p.15 / Chapter 2.1 --- "Formal Expression for G(x,y，w)" --- p.16 / Chapter 2.2 --- "Leaver's Series Solution: An Analytic Expression for g(r, w)" --- p.17 / Chapter 2.3 --- Location of the Cut --- p.22 / Chapter 2.4 --- "Jaffe's Series Solution: An Analytic Expression for f(r,w)" --- p.23 / Chapter 2.5 --- QNMs and Their Locations --- p.26 / Chapter 2.5.1 --- Alternative definitions of QNM --- p.26 / Chapter 2.5.2 --- Methods of searching for QNMs --- p.28 / Chapter 2.5.3 --- Locations of QNMs --- p.29 / Chapter 2.6 --- Green's Function and Eigenspectra --- p.30 / Chapter 3 --- Normalization Function: Analytical Treatment --- p.34 / Chapter 3.1 --- Definition and Properties --- p.34 / Chapter 3.2 --- Analytic Approximations for --- p.36 / Chapter 3.3 --- Polar Perturbations --- p.39 / Chapter 4 --- Normalization Function: Numerical Treatment --- p.42 / Chapter 4.1 --- "Numerical Algorithm for g(x,w)" --- p.42 / Chapter 4.1.1 --- Method --- p.42 / Chapter 4.1.2 --- Equation governing R(z) --- p.45 / Chapter 4.1.3 --- "Equations governing A(x, z) and B(x, z)" --- p.45 / Chapter 4.2 --- "Numerical Algorithm for g(x, ´ؤw)" --- p.49 / Chapter 4.3 --- Numerical Result of q(γ) --- p.50 / Chapter 4.4 --- Comparison of Numerical Result with Analytic Approximations --- p.56 / Chapter 5 --- "Branch Cut Strength of G(x, y, w)" --- p.58 / Chapter 5.1 --- "Relation between q(γ) and ΔG(x,y, ´ؤiγ)" --- p.58 / Chapter 5.2 --- Proof of the Power Law --- p.60 / Chapter 5.3 --- "Numerical Results for ΔG(x, y, ´ؤiγ)" --- p.63 / Chapter 5.4 --- Study of a Physically Important Limit --- p.65 / Chapter 5.4.1 --- Limiting x and y --- p.65 / Chapter 5.4.2 --- Poles on the unphysical sheet --- p.69 / Chapter 5.4.3 --- Zerilli potential --- p.77 / Chapter 6 --- Conclusion --- p.81 / Chapter A --- Tortoise Coordinate --- p.84 / Chapter B --- Solution of the Generalized Coulomb Wave Equation --- p.86 / Chapter C --- Derivation of (5.1) --- p.88 / Bibliography --- p.89

This thesis describes electrical measurements performed on low dimensional p-type devices, fabricated from GaAs/AlGaAs heterostructures. The Coulomb interaction between holes is similar to that between electrons. However, the kinetic energy is suppressed, which makes interaction effects particularly important. Holes may also be used to study band structure effects which arise from spin-orbit coupling in the valence band. The effects of Coulomb interactions in low dimensional electron systems are currently being studied extensively. Experiments presented in this thesis indicate the possible importance of Coulomb exchange interactions in both one and two dimensional hole systems (1DHSs,2DHSs). Tilted magnetic field studies of 2DHSs in the quantum Hall regime indicate that Landau levels at even filling factors will not cross. For high filling factor, this is attributed to a spin-orbit mixing effect which arises from the low symmetry ofthe system. At lower filling factor, activation-energy measurements verify that the energy gaps decrease and then increase as the field is tilted. However, the energy gap versus field dependences do not exhibit the curvature that might be expected from a perturbative anticrossing. It is speculated that the origin of this effect is a phase transition driven by the exchange interaction. Balanced arguments contrasting the relative strengths of the mixing and interactions theories are provided. The second part of this thesis describes a new method for the fabrication ofballistic 1DHSs, which exhibit clear conductance quantization. The quantization changes from even to odd multiples of e2/h as a function of the magnetic field in the plane of the heterostructure, as 'spin splitting' causes the 1D subbands to cross. Measurements of the 1D subband energy spacings are used together with the magnetic fields at which the crossings occur to calculate the in-plane g factors of the 1D subbands. These are found to increase as the number of occupied 1D subbands decreases. This enhancement of the g factor is attributed to exchange interactions; possible mixing explanations are also discussed. At higher magnetic fields, the pattern of quantization features shows that the subbands have crossed many times, and that the 1DHS can be strongly magnetized.

This dissertation investigates the signatures of electromagnetic radiation that may accompany two specific sources of gravitational radiation: the inspiral and merger of massive black hole binaries (MBHBs) in galactic nuclei, and the coalescence of black hole neutron star (BHNS) pairs. Part I considers the interaction of MBHBs, at sub-pc separations, with a circumbinary gas disk. Accretion rates onto the MBHB are calculated from two-dimensional hydrodynamical simulations as a function of the relative masses of the black holes. The results are applied to interpretation of the recent, sub-pc separation MBHB candidate in the nucleus of the periodically variable Quasar PG 1302-102. We advance an interpretation of the variability observed in PG 1302-102 as being caused by Doppler-boosted emission sourced by the orbital velocity of the smaller black hole in a MBHB with disparate relative masses. Part II considers BHNS binaries in which the black hole is large enough to swallow the neutron star whole before it is disrupted. As the pair nears merger, orbital motion of the black hole through the magnetosphere of the neutron star generates an electromotive force, a black-hole-battery, which, for the strongest neutron star magnetic field strengths, could power luminosities large enough to make the merging pair observable out to cosmic distances. Relativistic solutions for vacuum fields of a magnetic dipole near a horizon are given, and a mechanism for harnessing the power of the black-hole-battery is put forth in the form of a fireball emitting in hard X-rays to to gamma-rays.

Este trabalho visa o estudo das perturbações de sistemas gravitacionais altamente compactos, como buracos negros e estrelas de nêutrons e de quarks. As perturbações em questão podem ser de diversas naturezas (escalar, eletromagnética ou gravitacional), sendo que detivemo-nos mais atentamente naquelas de natureza gravitacional, pois estas têm despertado mais interesse por serem astronomicamente mais fáceis de detectar. Além de estudarmos tais perturbações, procedemos a uma comparação dos resultados para buracos negros, estrelas de nêutrons e de quarks. Tal comparação justifica-se pelo fato de que a confrontação de previsões teóricas com resultados experimentais pode ajudar-nos a identificar objetos astronômicos de interesse, distingüi-los e, no caso de estrelas, aprender algo sobre sua estrutura interna, particularmente sobre a equação de estado (EDE) do fluido estelar. No que se segue, dividimos o trabalho em sete partes. Em primeiro lugar, damos uma introdução bastante sucinta ao mesmo (Capítulo 1). Depois, falamos sobre a física de estrelas de nêutrons e de quarks (Capítulo 2). A seguir, fazemos um estudo comparativo dos dois tipos de estrelas (Capítulo 3). Mais adiante, discutimos as perturbações de diversos tipos, além de definir os MQNs (Modos Quasi-Normais) de buracos negros de Schwarzschild (Capítulo 4). Prosseguimos a discussão com a métrica de Reissner-Nordström-de Sitter (Capítulo 5) e introduzimos, na seqüência, os MQNs estelares, de forma muito breve (Capítulo 6). Por fim, apresentamos nossas conclusões (Capítulo 7). A parte inédita deste trabalho está concentrada nos capítulos 5 e 6, os quatro anteriores servindo de preparativo e de base comparativa para estes dois. / This work aims the detailed study of the perturbations of highly compact gravitational systems, such as black holes and both neutron and quark stars. Such perturbations may have several different characters, such as scalar and electromagnetic fields as well as gravitational (either axial or polar) disturbances. We have focused more closely on the latter kind of perturbation, since they offer better possibilities of detection in the near future, in the form of gravitational waves. Besides studying the aforementioned perturbations, we have proceeded to a comparison between black holes and neutron and quark stars , when it comes to the outcomes of the perturbations, usually called QNMs (quasi-normal modes). Such a comparison is actually in order, since a direct comparison of theoretical and observational data may help us identify astronomical objects and, in the case of compact stars, may provide valuable insights into these stars' inner structure, particularly when it comes to their equation of state (EOS). In what follows, we have subdivided this work in seven parts. We begin with a brief introduction (Chapter 1), then proceed to a description of the physics of both neutron and quark stars (Chapter 2) and, in the sequence, to a comparative study of both kinds of star (Chapter 3). Subsequently, we develop the perturbation theory of the Schwarzschild black holes, discussing their QNMs (Chapter 4) and doing the same, later, for a more general Reissner-Nordström-de Sitter geometry (chapter 5). After that, we provide a very brief introduction to the stellar MQNs (Chapter 6). Finally, we present our conclusions (Chapter 7). The chapters 5 and 6 carry the inedit part of this work, and the chapters from 1 to 4 pave the way and provide a comparative basis for them.

No contexto da teoria da relatividade geral de Einstein, se estudam espaço-tempos dinâmicos do tipo buraco negro em um ambiente cosmológico, em particular, uma generalização de massa variável do espaço-tempo de McVittie. São apresentados alguns espaço-tempos resultantes de limites da solução de McVittie generalizada. Se discutem as definições padrão de buraco negro e horizonte de eventos assim como as dificuldades de aplicá-las em situações dinâmicas, outras definições para horizontes são exploradas. É usado o conceito de horizonte aparente para localizar buracos negros e horizontes cosmológicos. Soluções para a busca dos horizontes aparentes são encontradas nas geometrias de Schwarzschild-de Sitter, McVittie e McVittie generalizado. / Black hole-like spacetimes in a cosmological background are studied within the Einsteins general relativity theory framework, in particular a mass varying generalization of the McVitties spacetime. We exhibit some of the resulting spacetimes as limit cases of the generalized McVittie solution. We discuss the standard definition of black hole and event horizon, and we address the difficulties in aplying it in dynamical situations, another definitions for horizons are explored. The apparent horizon concept is used to locate black holes and cosmological horizons. Solutions for apparent horizons in Schwarzschild-de Sitter, McVittie, and generalized McVittie geometries are shown.