Fonte escalar acoplada ao campo de Klein-Gordon orbitando um objeto estelar

Neste trabalho determinamos, utilizando Teoria Quântica de Campos em nível de árvore, a radiação escalar emitida por uma fonte em movimento circular uniforme no espaço-tempo plano de Minkowski, assumindo Gravitação Newtoniana, e no espaço-tempo curvo de um buraco negro sem carga e com momento angular nulo, assumindo Relatividade Geral. Efetuamos este cálculo analiticamente para o caso de Minkowski e numericamente no âmbito do espaço-tempo de Schwarzschild, sendo que neste espaço-tempo curvo obtivemos a forma analítica e a normalização dos modos nas regiões assintóticas. Verificamos que, para as órbitas circulares estáveis de acordo com a Relatividade Geral, a potência irradiada no caso de um buraco negro de Schwarzschild é menor do que a obtida no espaço-tempo de Minkowski assumindo a Gravitação Newtoniana. Obtemos também que apenas uma pequena parcela da radiação emitida é absorvida pelo buraco negro. Verificamos que a diferença entre as potências irradiadas em Schwarzschild e Minkowski diminui na medida em que aumentamos o valor da massa do campo. Em Schwarzschild, uma parcela cada vez maior da radiação emitida é absorvida pelo buraco negro na medida em que aumentamos o valor da massa do campo.

Domain wall description of superconductivity

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Campos espinoriais ELKO

Pós-graduação em Física - FEG

Multikink solutions and deformed defects

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Asymmetrical Bloch branes and the hierarchy problem

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Aplicações do fluxo de Ricci à teoria da relatividade geral: estudo dos buracos negros

The flow of Ricci is an analytical tool, and a similar equation for heat geometry, a diffusive process which acts on a variety of metrics Riemannian and thus can be used in mathematics to understand the topology of varieties and also in the study geometric theories. Thus, the Ricci curvature plays an important role in the General Theory of Relativity, characterized as a geometric theory, which is the dominant term in the Einstein field equations. The present work has as main objectives to develop and apply Ricci flow techniques to general relativity, in this case, a three-dimensional asymptotically flat Riemannian metric as a set of initial data for Einstein equations and establish relations and comparisons between them.

Galilean DKP theory and Bose-Einstein condensation

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Method for obtaining thick brane models

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

D-oscillons in the standard model extension

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Tópicos em teoria das perturbações cosmológicas

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Twinlike models for kinks and compactons in flat and warped spacetime

This work deals with the presence of twinlike models in scalar field theories. We show how to build distinct scalar field theories having the same extended solution, with the same energy density and linear stability. Here, however, we start from a given but generalized scalar field theory, and we construct the corresponding twin model, which also engenders generalized dynamics. We investigate how the twinlike models arise in both flat and curved spacetimes. In the curved spacetime, we consider a braneworld model with the warp factor controlling the spacetime geometry with a single extra dimension of infinite extent. In particular, we study linear stability in both flat and curved spacetimes, and in the case of curved spacetime-in both the gravity and the scalar field sectors-for the two braneworld models. DOI: 10.1103/PhysRevD.86.125021

Interactive quadrangulation with reeb atlases and connectivity textures

Creating high-quality quad meshes from triangulated surfaces is a highly nontrivial task that necessitates consideration of various application specific metrics of quality. In our work, we follow the premise that automatic reconstruction techniques may not generate outputs meeting all the subjective quality expectations of the user. Instead, we put the user at the center of the process by providing a flexible, interactive approach to quadrangulation design. By combining scalar field topology and combinatorial connectivity techniques, we present a new framework, following a coarse to fine design philosophy, which allows for explicit control of the subjective quality criteria on the output quad mesh, at interactive rates. Our quadrangulation framework uses the new notion of Reeb atlas editing, to define with a small amount of interactions a coarse quadrangulation of the model, capturing the main features of the shape, with user prescribed extraordinary vertices and alignment. Fine grain tuning is easily achieved with the notion of connectivity texturing, which allows for additional extraordinary vertices specification and explicit feature alignment, to capture the high-frequency geometries. Experiments demonstrate the interactivity and flexibility of our approach, as well as its ability to generate quad meshes of arbitrary resolution with high-quality statistics, while meeting the user's own subjective requirements.

Rotating black holes in a Randall-Sundrum brane with a cosmological constant

In this work we have constructed axially symmetric vacuum solutions of the gravitational field equations in a Randall-Sundrum brane. A non-null effective cosmological constant is considered, and asymptotically de Sitter and anti-de Sitter spacetimes are obtained. The solutions describe rotating black holes in a four-dimensional brane. Optical features of the solutions are treated, emphasizing the rotation of the polarization vector along null congruences. DOI: 10.1103/PhysRevD.86.124047

New cosmic accelerating scenario without dark energy

We propose an alternative, nonsingular, cosmic scenario based on gravitationally induced particle production. The model is an attempt to evade the coincidence and cosmological constant problems of the standard model (Lambda CDM) and also to connect the early and late time accelerating stages of the Universe. Our space-time emerges from a pure initial de Sitter stage thereby providing a natural solution to the horizon problem. Subsequently, due to an instability provoked by the production of massless particles, the Universe evolves smoothly to the standard radiation dominated era thereby ending the production of radiation as required by the conformal invariance. Next, the radiation becomes subdominant with the Universe entering in the cold dark matter dominated era. Finally, the negative pressure associated with the creation of cold dark matter (CCDM model) particles accelerates the expansion and drives the Universe to a final de Sitter stage. The late time cosmic expansion history of the CCDM model is exactly like in the standard Lambda CDM model; however, there is no dark energy. The model evolves between two limiting (early and late time) de Sitter regimes. All the stages are also discussed in terms of a scalar field description. This complete scenario is fully determined by two extreme energy densities, or equivalently, the associated de Sitter Hubble scales connected by rho(I)/rho(f) = (H-I/H-f)(2) similar to 10(122), a result that has no correlation with the cosmological constant problem. We also study the linear growth of matter perturbations at the final accelerating stage. It is found that the CCDM growth index can be written as a function of the Lambda growth index, gamma(Lambda) similar or equal to 6/11. In this framework, we also compare the observed growth rate of clustering with that predicted by the current CCDM model. Performing a chi(2) statistical test we show that the CCDM model provides growth rates that match sufficiently well with the observed growth rate of structure.

Exact cosmological solutions of models with an interacting dark sector

In this work we extend the first order formalism for cosmological models that present an interaction between a fermionic and a scalar field. Cosmological exact solutions describing universes filled with interacting dark energy and dark matter have been obtained. Viable cosmological solutions with an early period of decelerated expansion followed by late acceleration have been found, notably one which presents a dark matter component dominating in the past and a dark energy component dominating in the future. In another one, the dark energy alone is the responsible for both periods, similar to a Chaplygin gas case. Exclusively accelerating solutions have also been obtained.